1
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Cucinotta FA, Pak S. Cancer and circulatory disease risks for the largest solar particle events in the space age. LIFE SCIENCES IN SPACE RESEARCH 2024; 40:1-7. [PMID: 38245334 DOI: 10.1016/j.lssr.2023.10.003] [Citation(s) in RCA: 0] [Impact Index Per Article: 0] [Reference Citation Analysis] [Abstract] [Key Words] [MESH Headings] [Track Full Text] [Subscribe] [Scholar Register] [Received: 08/25/2023] [Revised: 10/23/2023] [Accepted: 10/24/2023] [Indexed: 01/22/2024]
Abstract
In this paper we use the NASA Space Cancer Risk (NSCR version 2022) model to predict cancer and circulatory disease risks using energy spectra representing the largest SPE's observed in the space age. Because tissue dose-rates behind shielding for large SPE's lead to low dose-rates (<0.2 Gy/h) we consider the integrated risk for several historical periods of high solar activity, including July-November, 1960 events and August-October 1989 events along with the February 1956 and August 1972 events. The galactic cosmic ray (GCR) contribution to risks is considered in predictions. Results for these largest historical events show risk of exposure induced death (REID) are mitigated to < 1.2 % with a 95 % confidence interval with passive radiation shielding of 20 g/cm2 aluminum, while larger amounts would support the application of the ALARA principle. Annual GCR risks are predicted to surpass the risks from large SPEs by ∼30 g/cm2 of aluminum shielding.
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Affiliation(s)
- Francis A Cucinotta
- Department of Health Physics and Diagnostic Sciences, University of Nevada, Las Vegas, NV, United States of America.
| | - Sungmin Pak
- Department of Health Physics and Diagnostic Sciences, University of Nevada, Las Vegas, NV, United States of America
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2
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Wu QT, Anderson H, Watkins AK, Arora D, Barnes K, Padovani M, Shingledecker CN, Arumainayagam CR, Battat JBR. Role of Low-Energy (<20 eV) Secondary Electrons in the Extraterrestrial Synthesis of Prebiotic Molecules. ACS EARTH & SPACE CHEMISTRY 2024; 8:79-88. [PMID: 38264085 PMCID: PMC10801738 DOI: 10.1021/acsearthspacechem.3c00259] [Citation(s) in RCA: 0] [Impact Index Per Article: 0] [Reference Citation Analysis] [Abstract] [Key Words] [Grants] [Track Full Text] [Figures] [Subscribe] [Scholar Register] [Received: 09/06/2023] [Revised: 11/27/2023] [Accepted: 11/29/2023] [Indexed: 01/25/2024]
Abstract
We demonstrate for the first time that Galactic cosmic rays with energies as high as ∼1010 eV can trigger a cascade of low-energy (<20 eV) secondary electrons that could be a significant contributor to the interstellar synthesis of prebiotic molecules whose delivery by comets, meteorites, and interplanetary dust particles may have kick-started life on Earth. For the energetic processing of interstellar ice mantles inside dark, dense molecular clouds, we explore the relative importance of low-energy (<20 eV) secondary electrons-agents of radiation chemistry-and low-energy (<10 eV), nonionizing photons-instigators of photochemistry. Our calculations indicate fluxes of ∼102 electrons cm-2 s-1 for low-energy secondary electrons produced within interstellar ices due to attenuated Galactic cosmic-ray protons. Consequently, in certain star-forming regions where internal high-energy radiation sources produce ionization rates that are observed to be a thousand times greater than the typical interstellar Galactic ionization rate, the flux of low-energy secondary electrons should far exceed that of nonionizing photons. Because reaction cross sections can be several orders of magnitude larger for electrons than for photons, even in the absence of such enhancement, our calculations indicate that secondary low-energy (<20 eV) electrons are at least as significant as low-energy (<10 eV) nonionizing photons in the interstellar synthesis of prebiotic molecules. Most importantly, our results demonstrate the pressing need for explicitly incorporating low-energy electrons in current and future astrochemical simulations of cosmic ices. Such models are critically important for interpreting James Webb Space Telescope infrared measurements, which are currently being used to probe the origins of life by studying complex organic molecules found in ices near star-forming regions.
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Affiliation(s)
- Qin Tong Wu
- Department
of Chemistry, Wellesley College, Wellesley, Massachusetts 02481, United States
| | - Hannah Anderson
- Department
of Chemistry, Wellesley College, Wellesley, Massachusetts 02481, United States
| | - Aurland K. Watkins
- Department
of Chemistry, Wellesley College, Wellesley, Massachusetts 02481, United States
| | - Devyani Arora
- Department
of Chemistry, Wellesley College, Wellesley, Massachusetts 02481, United States
| | - Kennedy Barnes
- Department
of Chemistry, Wellesley College, Wellesley, Massachusetts 02481, United States
| | - Marco Padovani
- INAF—Osservatorio
Astrofisico di Arcetri, Largo E. Fermi, 5, 50125 Firenze, Italy
| | | | | | - James B. R. Battat
- Department
of Physics & Astronomy, Wellesley College, Wellesley, Massachusetts 02481, United States
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3
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Ruszkowski M, Pfrommer C. Cosmic ray feedback in galaxies and galaxy clusters: A pedagogical introduction and a topical review of the acceleration, transport, observables, and dynamical impact of cosmic rays. THE ASTRONOMY AND ASTROPHYSICS REVIEW 2023; 31:4. [PMID: 38115816 PMCID: PMC10730010 DOI: 10.1007/s00159-023-00149-2] [Citation(s) in RCA: 0] [Impact Index Per Article: 0] [Reference Citation Analysis] [Abstract] [Key Words] [Grants] [Track Full Text] [Figures] [Subscribe] [Scholar Register] [Received: 06/05/2023] [Accepted: 10/05/2023] [Indexed: 12/21/2023]
Abstract
Understanding the physical mechanisms that control galaxy formation is a fundamental challenge in contemporary astrophysics. Recent advances in the field of astrophysical feedback strongly suggest that cosmic rays (CRs) may be crucially important for our understanding of cosmological galaxy formation and evolution. The appealing features of CRs are their relatively long cooling times and relatively strong dynamical coupling to the gas. In galaxies, CRs can be close to equipartition with the thermal, magnetic, and turbulent energy density in the interstellar medium, and can be dynamically very important in driving large-scale galactic winds. Similarly, CRs may provide a significant contribution to the pressure in the circumgalactic medium. In galaxy clusters, CRs may play a key role in addressing the classic cooling flow problem by facilitating efficient heating of the intracluster medium and preventing excessive star formation. Overall, the underlying physics of CR interactions with plasmas exhibit broad parallels across the entire range of scales characteristic of the interstellar, circumgalactic, and intracluster media. Here we present a review of the state-of-the-art of this field and provide a pedagogical introduction to cosmic ray plasma physics, including the physics of wave-particle interactions, acceleration processes, CR spatial and spectral transport, and important cooling processes. The field is ripe for discovery and will remain the subject of intense theoretical, computational, and observational research over the next decade with profound implications for the interpretation of the observations of stellar and supermassive black hole feedback spanning the entire width of the electromagnetic spectrum and multi-messenger data.
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Affiliation(s)
- Mateusz Ruszkowski
- Department of Astronomy, University of Michigan, 1085 S. University Ave., 323 West Hall, Ann Arbor, MI 48109-1107 USA
- Max Planck Institute for Astrophysics, Karl-Schwarzschild-Str. 1, 85748 Garching, Germany
| | - Christoph Pfrommer
- Leibniz Institute for Astrophysics Potsdam (AIP), An der Sternwarte 16, 14482 Potsdam, Germany
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4
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Oromiehie E, Nair V, Short K, Wei T, Bhattacharyya D, Prusty BG. Effect of He 2+ ion irradiation on the mechanical properties of automated fibre placement (AFP) CF-PEEK thermoplastics composites. Sci Rep 2023; 13:18787. [PMID: 37914794 PMCID: PMC10620137 DOI: 10.1038/s41598-023-45742-8] [Citation(s) in RCA: 0] [Impact Index Per Article: 0] [Reference Citation Analysis] [Abstract] [Key Words] [Grants] [Track Full Text] [Journal Information] [Subscribe] [Scholar Register] [Received: 06/06/2023] [Accepted: 10/23/2023] [Indexed: 11/03/2023] Open
Abstract
Carbon fibre-reinforced polyetheretherketone (CF-PEEK) composites have gained significant usage across diverse industries like automotive and aerospace due to their desirable characteristics. These properties encompass recyclability, low density, high strength, wear resistance and thermal stability. The components made from CF-PEEK composites for space applications will be subjected to a high radiation environment due to the incoming cosmic rays, comprising protons, α particles, electrons, γ rays, etc., once they escape the Earth's atmosphere. The ion irradiation of CF-PEEK is accompanied by radiation-induced effects, which drastically change the structure and properties of irradiated material. Since the resistance of CF-PEEK to radiation damage has not been studied extensively, this study aims to understand the effect of high-energy He2+ ions on the microstructure and properties of CF-PEEK composites manufactured using automated fibre placement (AFP) under different processing conditions. The samples have been radiated with 5 MeV He2+ ions using an energy degrader wheel to create a layer with relatively uniform damage. Then, were characterized using optical and scanning electron microscopy and their hardness was evaluated using nanoindentation. It was observed that, irradiation increases the hardness of the fibres in all cases. Also, fibre orientation affects the hardness in a statistically significant manner in both unirradiated and irradiated conditions.
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Affiliation(s)
- Ebrahim Oromiehie
- ARC Training Centre for Automated Manufacture of Advanced Composites, School of Mechanical and Manufacturing Engineering, UNSW Sydney, Sydney, NSW, 2052, Australia.
| | - Vishnu Nair
- School of Mechanical and Manufacturing Engineering, UNSW Sydney, Sydney, NSW, 2052, Australia
| | - Ken Short
- Australian Nuclear Science and Technology Organization (ANSTO), Lucas Heights, NSW, 2234, Australia
| | - Tao Wei
- Australian Nuclear Science and Technology Organization (ANSTO), Lucas Heights, NSW, 2234, Australia
| | - Dhriti Bhattacharyya
- Australian Nuclear Science and Technology Organization (ANSTO), Lucas Heights, NSW, 2234, Australia
- School of Materials Science and Engineering, UNSW Sydney, Sydney, NSW, 2052, Australia
| | - B Gangadhara Prusty
- ARC Training Centre for Automated Manufacture of Advanced Composites, School of Mechanical and Manufacturing Engineering, UNSW Sydney, Sydney, NSW, 2052, Australia
- Sovereign Manufacturing Automation for Composites CRC Ltd (SOMAC CRC), Sydney, NSW, 2052, Australia
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5
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Aguilar M, Ali Cavasonza L, Alpat B, Ambrosi G, Arruda L, Attig N, Bagwell C, Barao F, Barrin L, Bartoloni A, Başeğmez-du Pree S, Battiston R, Belyaev N, Berdugo J, Bertucci B, Bindi V, Bollweg K, Bolster J, Borchiellini M, Borgia B, Boschini MJ, Bourquin M, Bueno EF, Burger J, Burger WJ, Cai XD, Capell M, Casaus J, Castellini G, Cervelli F, Chang YH, Chen GM, Chen GR, Chen H, Chen HS, Chen Y, Cheng L, Chou HY, Chouridou S, Choutko V, Chung CH, Clark C, Coignet G, Consolandi C, Contin A, Corti C, Cui Z, Dadzie K, Dass A, Delgado C, Della Torre S, Demirköz MB, Derome L, Di Falco S, Di Felice V, Díaz C, Dimiccoli F, von Doetinchem P, Dong F, Donnini F, Duranti M, Egorov A, Eline A, Faldi F, Feng J, Fiandrini E, Fisher P, Formato V, Gámez C, García-López RJ, Gargiulo C, Gast H, Gervasi M, Giovacchini F, Gómez-Coral DM, Gong J, Goy C, Grabski V, Grandi D, Graziani M, Guracho AN, Haino S, Han KC, Hashmani RK, He ZH, Heber B, Hsieh TH, Hu JY, Huang BW, Incagli M, Jang WY, Jia Y, Jinchi H, Karagöz G, Khiali B, Kim GN, Kirn T, Kounina O, Kounine A, Koutsenko V, Krasnopevtsev D, Kuhlman A, Kulemzin A, La Vacca G, Laudi E, Laurenti G, LaVecchia G, Lazzizzera I, Lee HT, Lee SC, Li HL, Li JQ, Li M, Li M, Li Q, Li Q, Li QY, Li S, Li SL, Li JH, Li ZH, Liang J, Liang MJ, Lin CH, Lippert T, Liu JH, Lu SQ, Lu YS, Luebelsmeyer K, Luo JZ, Luo SD, Luo X, Machate F, Mañá C, Marín J, Marquardt J, Martin T, Martínez G, Masi N, Maurin D, Medvedeva T, Menchaca-Rocha A, Meng Q, Mikhailov VV, Molero M, Mott P, Mussolin L, Negrete J, Nikonov N, Nozzoli F, Ocampo-Peleteiro J, Oliva A, Orcinha M, Ottupara MA, Palermo M, Palmonari F, Paniccia M, Pashnin A, Pauluzzi M, Pensotti S, Plyaskin V, Poluianov S, Qin X, Qu ZY, Quadrani L, Rancoita PG, Rapin D, Reina Conde A, Robyn E, Romaneehsen L, Rozhkov A, Rozza D, Sagdeev R, Schael S, Schultz von Dratzig A, Schwering G, Seo ES, Shan BS, Siedenburg T, Song JW, Song XJ, Sonnabend R, Strigari L, Su T, Sun Q, Sun ZT, Tacconi M, Tang XW, Tang ZC, Tian J, Tian Y, Ting SCC, Ting SM, Tomassetti N, Torsti J, Urban T, Usoskin I, Vagelli V, Vainio R, Valencia-Otero M, Valente E, Valtonen E, Vázquez Acosta M, Vecchi M, Velasco M, Vialle JP, Wang CX, Wang L, Wang LQ, Wang NH, Wang QL, Wang S, Wang X, Wang Y, Wang ZM, Wei J, Weng ZL, Wu H, Wu Y, Xiao JN, Xiong RQ, Xiong XZ, Xu W, Yan Q, Yang HT, Yang Y, Yashin II, Yelland A, Yi H, You YH, Yu YM, Yu ZQ, Zannoni M, Zhang C, Zhang F, Zhang FZ, Zhang J, Zhang JH, Zhang Z, Zhao F, Zheng C, Zheng ZM, Zhuang HL, Zhukov V, Zichichi A, Zuccon P. Properties of Cosmic-Ray Sulfur and Determination of the Composition of Primary Cosmic-Ray Carbon, Neon, Magnesium, and Sulfur: Ten-Year Results from the Alpha Magnetic Spectrometer. PHYSICAL REVIEW LETTERS 2023; 130:211002. [PMID: 37295095 DOI: 10.1103/physrevlett.130.211002] [Citation(s) in RCA: 0] [Impact Index Per Article: 0] [Reference Citation Analysis] [Abstract] [Track Full Text] [Subscribe] [Scholar Register] [Received: 02/09/2023] [Revised: 03/28/2023] [Accepted: 04/27/2023] [Indexed: 06/12/2023]
Abstract
We report the properties of primary cosmic-ray sulfur (S) in the rigidity range 2.15 GV to 3.0 TV based on 0.38×10^{6} sulfur nuclei collected by the Alpha Magnetic Spectrometer experiment (AMS). We observed that above 90 GV the rigidity dependence of the S flux is identical to the rigidity dependence of Ne-Mg-Si fluxes, which is different from the rigidity dependence of the He-C-O-Fe fluxes. We found that, similar to N, Na, and Al cosmic rays, over the entire rigidity range, the traditional primary cosmic rays S, Ne, Mg, and C all have sizeable secondary components, and the S, Ne, and Mg fluxes are well described by the weighted sum of the primary silicon flux and the secondary fluorine flux, and the C flux is well described by the weighted sum of the primary oxygen flux and the secondary boron flux. The primary and secondary contributions of the traditional primary cosmic-ray fluxes of C, Ne, Mg, and S (even Z elements) are distinctly different from the primary and secondary contributions of the N, Na, and Al (odd Z elements) fluxes. The abundance ratio at the source for S/Si is 0.167±0.006, for Ne/Si is 0.833±0.025, for Mg/Si is 0.994±0.029, and for C/O is 0.836±0.025. These values are determined independent of cosmic-ray propagation.
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Affiliation(s)
- M Aguilar
- Centro de Investigaciones Energéticas, Medioambientales y Tecnológicas (CIEMAT), 28040 Madrid, Spain
| | - L Ali Cavasonza
- I. Physics Institute and JARA-FAME, RWTH Aachen University, 52056 Aachen, Germany
| | - B Alpat
- INFN Sezione di Perugia, 06100 Perugia, Italy
| | - G Ambrosi
- INFN Sezione di Perugia, 06100 Perugia, Italy
| | - L Arruda
- Laboratório de Instrumentação e Física Experimental de Partículas (LIP), 1649-003 Lisboa, Portugal
| | - N Attig
- Jülich Supercomputing Centre and JARA-FAME, Research Centre Jülich, 52425 Jülich, Germany
| | - C Bagwell
- Massachusetts Institute of Technology (MIT), Cambridge, Massachusetts 02139, USA
| | - F Barao
- Laboratório de Instrumentação e Física Experimental de Partículas (LIP), 1649-003 Lisboa, Portugal
| | - L Barrin
- European Organization for Nuclear Research (CERN), 1211 Geneva 23, Switzerland
| | | | - S Başeğmez-du Pree
- Kapteyn Astronomical Institute, University of Groningen, P.O. Box 800, 9700 AV Groningen, Netherlands
| | - R Battiston
- INFN TIFPA, 38123 Trento, Italy
- Università di Trento, 38123 Trento, Italy
| | - N Belyaev
- Massachusetts Institute of Technology (MIT), Cambridge, Massachusetts 02139, USA
| | - J Berdugo
- Centro de Investigaciones Energéticas, Medioambientales y Tecnológicas (CIEMAT), 28040 Madrid, Spain
| | - B Bertucci
- INFN Sezione di Perugia, 06100 Perugia, Italy
- Università di Perugia, 06100 Perugia, Italy
| | - V Bindi
- Physics and Astronomy Department, University of Hawaii, Honolulu, Hawaii 96822, USA
| | - K Bollweg
- National Aeronautics and Space Administration Johnson Space Center (JSC), Houston, Texas 77058, USA
| | - J Bolster
- Massachusetts Institute of Technology (MIT), Cambridge, Massachusetts 02139, USA
| | - M Borchiellini
- Kapteyn Astronomical Institute, University of Groningen, P.O. Box 800, 9700 AV Groningen, Netherlands
| | - B Borgia
- INFN Sezione di Roma 1, 00185 Roma, Italy
- Università di Roma La Sapienza, 00185 Roma, Italy
| | - M J Boschini
- INFN Sezione di Milano-Bicocca, 20126 Milano, Italy
| | - M Bourquin
- DPNC, Université de Genève, 1211 Genève 4, Switzerland
| | - E F Bueno
- Kapteyn Astronomical Institute, University of Groningen, P.O. Box 800, 9700 AV Groningen, Netherlands
| | - J Burger
- Massachusetts Institute of Technology (MIT), Cambridge, Massachusetts 02139, USA
| | | | - X D Cai
- Massachusetts Institute of Technology (MIT), Cambridge, Massachusetts 02139, USA
| | - M Capell
- Massachusetts Institute of Technology (MIT), Cambridge, Massachusetts 02139, USA
| | - J Casaus
- Centro de Investigaciones Energéticas, Medioambientales y Tecnológicas (CIEMAT), 28040 Madrid, Spain
| | | | | | - Y H Chang
- Institute of Physics, Academia Sinica, Nankang, Taipei 11529, Taiwan
| | - G M Chen
- Institute of High Energy Physics (IHEP), Chinese Academy of Sciences, Beijing 100049, China
- University of Chinese Academy of Sciences (UCAS), Beijing 100049, China
| | - G R Chen
- Shandong Institute of Advanced Technology (SDIAT), Jinan, Shandong 250100, China
| | - H Chen
- Zhejiang University (ZJU), Hangzhou 310058, China
| | - H S Chen
- Institute of High Energy Physics (IHEP), Chinese Academy of Sciences, Beijing 100049, China
- University of Chinese Academy of Sciences (UCAS), Beijing 100049, China
| | - Y Chen
- DPNC, Université de Genève, 1211 Genève 4, Switzerland
- Shandong Institute of Advanced Technology (SDIAT), Jinan, Shandong 250100, China
| | - L Cheng
- Shandong Institute of Advanced Technology (SDIAT), Jinan, Shandong 250100, China
| | - H Y Chou
- Institute of Physics, Academia Sinica, Nankang, Taipei 11529, Taiwan
| | - S Chouridou
- I. Physics Institute and JARA-FAME, RWTH Aachen University, 52056 Aachen, Germany
| | - V Choutko
- Massachusetts Institute of Technology (MIT), Cambridge, Massachusetts 02139, USA
| | - C H Chung
- I. Physics Institute and JARA-FAME, RWTH Aachen University, 52056 Aachen, Germany
| | - C Clark
- Massachusetts Institute of Technology (MIT), Cambridge, Massachusetts 02139, USA
- National Aeronautics and Space Administration Johnson Space Center (JSC), Houston, Texas 77058, USA
| | - G Coignet
- Université Grenoble Alpes, Université Savoie Mont Blanc, CNRS, LAPP-IN2P3, 74000 Annecy, France
| | - C Consolandi
- Physics and Astronomy Department, University of Hawaii, Honolulu, Hawaii 96822, USA
| | - A Contin
- INFN Sezione di Bologna, 40126 Bologna, Italy
- Università di Bologna, 40126 Bologna, Italy
| | - C Corti
- Physics and Astronomy Department, University of Hawaii, Honolulu, Hawaii 96822, USA
| | - Z Cui
- Shandong University (SDU), Jinan, Shandong 250100, China
- Shandong Institute of Advanced Technology (SDIAT), Jinan, Shandong 250100, China
| | - K Dadzie
- Massachusetts Institute of Technology (MIT), Cambridge, Massachusetts 02139, USA
| | - A Dass
- INFN TIFPA, 38123 Trento, Italy
- Università di Trento, 38123 Trento, Italy
| | - C Delgado
- Centro de Investigaciones Energéticas, Medioambientales y Tecnológicas (CIEMAT), 28040 Madrid, Spain
| | | | - M B Demirköz
- Department of Physics, Middle East Technical University (METU), 06800 Ankara, Türkiye
| | - L Derome
- Université Grenoble Alpes, CNRS, Grenoble INP, LPSC-IN2P3, 38000 Grenoble, France
| | | | - V Di Felice
- INFN Sezione di Roma Tor Vergata, 00133 Roma, Italy
| | - C Díaz
- Centro de Investigaciones Energéticas, Medioambientales y Tecnológicas (CIEMAT), 28040 Madrid, Spain
| | | | - P von Doetinchem
- Physics and Astronomy Department, University of Hawaii, Honolulu, Hawaii 96822, USA
| | - F Dong
- Southeast University (SEU), Nanjing 210096, China
| | - F Donnini
- INFN Sezione di Perugia, 06100 Perugia, Italy
| | - M Duranti
- INFN Sezione di Perugia, 06100 Perugia, Italy
| | - A Egorov
- Massachusetts Institute of Technology (MIT), Cambridge, Massachusetts 02139, USA
| | - A Eline
- Massachusetts Institute of Technology (MIT), Cambridge, Massachusetts 02139, USA
| | - F Faldi
- INFN Sezione di Perugia, 06100 Perugia, Italy
- Università di Perugia, 06100 Perugia, Italy
| | - J Feng
- Sun Yat-Sen University (SYSU), Guangzhou 510275, China
| | - E Fiandrini
- INFN Sezione di Perugia, 06100 Perugia, Italy
- Università di Perugia, 06100 Perugia, Italy
| | - P Fisher
- Massachusetts Institute of Technology (MIT), Cambridge, Massachusetts 02139, USA
| | - V Formato
- INFN Sezione di Roma Tor Vergata, 00133 Roma, Italy
| | - C Gámez
- Centro de Investigaciones Energéticas, Medioambientales y Tecnológicas (CIEMAT), 28040 Madrid, Spain
| | - R J García-López
- Instituto de Astrofísica de Canarias (IAC), 38205 La Laguna, and Departamento de Astrofísica, Universidad de La Laguna, 38206 La Laguna, Tenerife, Spain
| | - C Gargiulo
- European Organization for Nuclear Research (CERN), 1211 Geneva 23, Switzerland
| | - H Gast
- I. Physics Institute and JARA-FAME, RWTH Aachen University, 52056 Aachen, Germany
| | - M Gervasi
- INFN Sezione di Milano-Bicocca, 20126 Milano, Italy
- Università di Milano-Bicocca, 20126 Milano, Italy
| | - F Giovacchini
- Centro de Investigaciones Energéticas, Medioambientales y Tecnológicas (CIEMAT), 28040 Madrid, Spain
| | - D M Gómez-Coral
- Physics and Astronomy Department, University of Hawaii, Honolulu, Hawaii 96822, USA
| | - J Gong
- Southeast University (SEU), Nanjing 210096, China
| | - C Goy
- Université Grenoble Alpes, Université Savoie Mont Blanc, CNRS, LAPP-IN2P3, 74000 Annecy, France
| | - V Grabski
- Instituto de Física, Universidad Nacional Autónoma de México (UNAM), Ciudad de México, 01000 Mexico
| | - D Grandi
- INFN Sezione di Milano-Bicocca, 20126 Milano, Italy
- Università di Milano-Bicocca, 20126 Milano, Italy
| | - M Graziani
- INFN Sezione di Perugia, 06100 Perugia, Italy
- Università di Perugia, 06100 Perugia, Italy
| | | | - S Haino
- Institute of Physics, Academia Sinica, Nankang, Taipei 11529, Taiwan
| | - K C Han
- National Chung-Shan Institute of Science and Technology (NCSIST), Longtan, Tao Yuan 32546, Taiwan
| | - R K Hashmani
- Department of Physics, Middle East Technical University (METU), 06800 Ankara, Türkiye
| | - Z H He
- Sun Yat-Sen University (SYSU), Guangzhou 510275, China
| | - B Heber
- Institut für Experimentelle und Angewandte Physik, Christian-Alberts-Universität zu Kiel, 24118 Kiel, Germany
| | - T H Hsieh
- Massachusetts Institute of Technology (MIT), Cambridge, Massachusetts 02139, USA
| | - J Y Hu
- Institute of High Energy Physics (IHEP), Chinese Academy of Sciences, Beijing 100049, China
- University of Chinese Academy of Sciences (UCAS), Beijing 100049, China
| | - B W Huang
- Zhejiang University (ZJU), Hangzhou 310058, China
| | - M Incagli
- INFN Sezione di Pisa, 56100 Pisa, Italy
| | - W Y Jang
- CHEP, Kyungpook National University, 41566 Daegu, Korea
| | - Yi Jia
- Massachusetts Institute of Technology (MIT), Cambridge, Massachusetts 02139, USA
| | - H Jinchi
- National Chung-Shan Institute of Science and Technology (NCSIST), Longtan, Tao Yuan 32546, Taiwan
| | - G Karagöz
- Department of Physics, Middle East Technical University (METU), 06800 Ankara, Türkiye
| | - B Khiali
- INFN Sezione di Roma Tor Vergata, 00133 Roma, Italy
| | - G N Kim
- CHEP, Kyungpook National University, 41566 Daegu, Korea
| | - Th Kirn
- I. Physics Institute and JARA-FAME, RWTH Aachen University, 52056 Aachen, Germany
| | - O Kounina
- Massachusetts Institute of Technology (MIT), Cambridge, Massachusetts 02139, USA
| | - A Kounine
- Massachusetts Institute of Technology (MIT), Cambridge, Massachusetts 02139, USA
| | - V Koutsenko
- Massachusetts Institute of Technology (MIT), Cambridge, Massachusetts 02139, USA
| | - D Krasnopevtsev
- Massachusetts Institute of Technology (MIT), Cambridge, Massachusetts 02139, USA
| | - A Kuhlman
- Physics and Astronomy Department, University of Hawaii, Honolulu, Hawaii 96822, USA
| | - A Kulemzin
- Massachusetts Institute of Technology (MIT), Cambridge, Massachusetts 02139, USA
| | - G La Vacca
- INFN Sezione di Milano-Bicocca, 20126 Milano, Italy
- Università di Milano-Bicocca, 20126 Milano, Italy
| | - E Laudi
- European Organization for Nuclear Research (CERN), 1211 Geneva 23, Switzerland
| | - G Laurenti
- INFN Sezione di Bologna, 40126 Bologna, Italy
| | - G LaVecchia
- Massachusetts Institute of Technology (MIT), Cambridge, Massachusetts 02139, USA
| | - I Lazzizzera
- INFN TIFPA, 38123 Trento, Italy
- Università di Trento, 38123 Trento, Italy
| | - H T Lee
- Academia Sinica Grid Center (ASGC), Nankang, Taipei 11529, Taiwan
| | - S C Lee
- Institute of Physics, Academia Sinica, Nankang, Taipei 11529, Taiwan
| | - H L Li
- Shandong Institute of Advanced Technology (SDIAT), Jinan, Shandong 250100, China
| | - J Q Li
- Southeast University (SEU), Nanjing 210096, China
| | - M Li
- I. Physics Institute and JARA-FAME, RWTH Aachen University, 52056 Aachen, Germany
- DPNC, Université de Genève, 1211 Genève 4, Switzerland
| | - M Li
- Shandong University (SDU), Jinan, Shandong 250100, China
| | - Q Li
- Southeast University (SEU), Nanjing 210096, China
| | - Q Li
- Shandong University (SDU), Jinan, Shandong 250100, China
| | - Q Y Li
- Shandong Institute of Advanced Technology (SDIAT), Jinan, Shandong 250100, China
| | - S Li
- I. Physics Institute and JARA-FAME, RWTH Aachen University, 52056 Aachen, Germany
| | - S L Li
- Institute of High Energy Physics (IHEP), Chinese Academy of Sciences, Beijing 100049, China
- University of Chinese Academy of Sciences (UCAS), Beijing 100049, China
| | - J H Li
- Shandong University (SDU), Jinan, Shandong 250100, China
| | - Z H Li
- Institute of High Energy Physics (IHEP), Chinese Academy of Sciences, Beijing 100049, China
- University of Chinese Academy of Sciences (UCAS), Beijing 100049, China
| | - J Liang
- Shandong University (SDU), Jinan, Shandong 250100, China
| | - M J Liang
- Institute of High Energy Physics (IHEP), Chinese Academy of Sciences, Beijing 100049, China
- University of Chinese Academy of Sciences (UCAS), Beijing 100049, China
| | - C H Lin
- Institute of Physics, Academia Sinica, Nankang, Taipei 11529, Taiwan
| | - T Lippert
- Jülich Supercomputing Centre and JARA-FAME, Research Centre Jülich, 52425 Jülich, Germany
| | - J H Liu
- Institute of Electrical Engineering (IEE), Chinese Academy of Sciences, Beijing 100190, China
| | - S Q Lu
- Institute of Physics, Academia Sinica, Nankang, Taipei 11529, Taiwan
| | - Y S Lu
- Institute of High Energy Physics (IHEP), Chinese Academy of Sciences, Beijing 100049, China
| | - K Luebelsmeyer
- I. Physics Institute and JARA-FAME, RWTH Aachen University, 52056 Aachen, Germany
| | - J Z Luo
- Southeast University (SEU), Nanjing 210096, China
| | - S D Luo
- Zhejiang University (ZJU), Hangzhou 310058, China
| | - Xi Luo
- Shandong Institute of Advanced Technology (SDIAT), Jinan, Shandong 250100, China
| | - F Machate
- I. Physics Institute and JARA-FAME, RWTH Aachen University, 52056 Aachen, Germany
| | - C Mañá
- Centro de Investigaciones Energéticas, Medioambientales y Tecnológicas (CIEMAT), 28040 Madrid, Spain
| | - J Marín
- Centro de Investigaciones Energéticas, Medioambientales y Tecnológicas (CIEMAT), 28040 Madrid, Spain
| | - J Marquardt
- Institut für Experimentelle und Angewandte Physik, Christian-Alberts-Universität zu Kiel, 24118 Kiel, Germany
| | - T Martin
- Massachusetts Institute of Technology (MIT), Cambridge, Massachusetts 02139, USA
- National Aeronautics and Space Administration Johnson Space Center (JSC), Houston, Texas 77058, USA
| | - G Martínez
- Centro de Investigaciones Energéticas, Medioambientales y Tecnológicas (CIEMAT), 28040 Madrid, Spain
| | - N Masi
- INFN Sezione di Bologna, 40126 Bologna, Italy
| | - D Maurin
- Université Grenoble Alpes, CNRS, Grenoble INP, LPSC-IN2P3, 38000 Grenoble, France
| | - T Medvedeva
- Massachusetts Institute of Technology (MIT), Cambridge, Massachusetts 02139, USA
| | - A Menchaca-Rocha
- Instituto de Física, Universidad Nacional Autónoma de México (UNAM), Ciudad de México, 01000 Mexico
| | - Q Meng
- Southeast University (SEU), Nanjing 210096, China
| | - V V Mikhailov
- NRNU MEPhI (Moscow Engineering Physics Institute), Moscow, 115409 Russia
| | - M Molero
- Instituto de Astrofísica de Canarias (IAC), 38205 La Laguna, and Departamento de Astrofísica, Universidad de La Laguna, 38206 La Laguna, Tenerife, Spain
| | - P Mott
- Massachusetts Institute of Technology (MIT), Cambridge, Massachusetts 02139, USA
- National Aeronautics and Space Administration Johnson Space Center (JSC), Houston, Texas 77058, USA
| | - L Mussolin
- INFN Sezione di Perugia, 06100 Perugia, Italy
- Università di Perugia, 06100 Perugia, Italy
| | - J Negrete
- Physics and Astronomy Department, University of Hawaii, Honolulu, Hawaii 96822, USA
| | - N Nikonov
- Physics and Astronomy Department, University of Hawaii, Honolulu, Hawaii 96822, USA
| | | | - J Ocampo-Peleteiro
- Centro de Investigaciones Energéticas, Medioambientales y Tecnológicas (CIEMAT), 28040 Madrid, Spain
| | - A Oliva
- INFN Sezione di Bologna, 40126 Bologna, Italy
| | - M Orcinha
- Laboratório de Instrumentação e Física Experimental de Partículas (LIP), 1649-003 Lisboa, Portugal
| | - M A Ottupara
- Shandong Institute of Advanced Technology (SDIAT), Jinan, Shandong 250100, China
| | - M Palermo
- Physics and Astronomy Department, University of Hawaii, Honolulu, Hawaii 96822, USA
| | - F Palmonari
- INFN Sezione di Bologna, 40126 Bologna, Italy
- Università di Bologna, 40126 Bologna, Italy
| | - M Paniccia
- DPNC, Université de Genève, 1211 Genève 4, Switzerland
| | - A Pashnin
- Massachusetts Institute of Technology (MIT), Cambridge, Massachusetts 02139, USA
| | - M Pauluzzi
- INFN Sezione di Perugia, 06100 Perugia, Italy
- Università di Perugia, 06100 Perugia, Italy
| | - S Pensotti
- INFN Sezione di Milano-Bicocca, 20126 Milano, Italy
- Università di Milano-Bicocca, 20126 Milano, Italy
| | - V Plyaskin
- Massachusetts Institute of Technology (MIT), Cambridge, Massachusetts 02139, USA
| | - S Poluianov
- Sodankylä Geophysical Observatory and Space Physics and Astronomy Research Unit, University of Oulu, 90014 Oulu, Finland
| | - X Qin
- Massachusetts Institute of Technology (MIT), Cambridge, Massachusetts 02139, USA
| | - Z Y Qu
- Shandong Institute of Advanced Technology (SDIAT), Jinan, Shandong 250100, China
| | - L Quadrani
- INFN Sezione di Bologna, 40126 Bologna, Italy
- Università di Bologna, 40126 Bologna, Italy
| | - P G Rancoita
- INFN Sezione di Milano-Bicocca, 20126 Milano, Italy
| | - D Rapin
- DPNC, Université de Genève, 1211 Genève 4, Switzerland
| | | | - E Robyn
- DPNC, Université de Genève, 1211 Genève 4, Switzerland
| | - L Romaneehsen
- Institut für Experimentelle und Angewandte Physik, Christian-Alberts-Universität zu Kiel, 24118 Kiel, Germany
| | - A Rozhkov
- Massachusetts Institute of Technology (MIT), Cambridge, Massachusetts 02139, USA
| | - D Rozza
- INFN Sezione di Milano-Bicocca, 20126 Milano, Italy
| | - R Sagdeev
- East-West Center for Space Science, University of Maryland, College Park, Maryland 20742, USA
| | - S Schael
- I. Physics Institute and JARA-FAME, RWTH Aachen University, 52056 Aachen, Germany
| | | | - G Schwering
- I. Physics Institute and JARA-FAME, RWTH Aachen University, 52056 Aachen, Germany
| | - E S Seo
- IPST, University of Maryland, College Park, Maryland 20742, USA
| | - B S Shan
- Beihang University (BUAA), Beijing 100191, China
| | - T Siedenburg
- I. Physics Institute and JARA-FAME, RWTH Aachen University, 52056 Aachen, Germany
| | - J W Song
- Shandong University (SDU), Jinan, Shandong 250100, China
| | - X J Song
- Shandong Institute of Advanced Technology (SDIAT), Jinan, Shandong 250100, China
| | - R Sonnabend
- I. Physics Institute and JARA-FAME, RWTH Aachen University, 52056 Aachen, Germany
| | - L Strigari
- INFN Sezione di Roma 1, 00185 Roma, Italy
| | - T Su
- Shandong Institute of Advanced Technology (SDIAT), Jinan, Shandong 250100, China
| | - Q Sun
- Shandong University (SDU), Jinan, Shandong 250100, China
| | - Z T Sun
- Institute of High Energy Physics (IHEP), Chinese Academy of Sciences, Beijing 100049, China
- University of Chinese Academy of Sciences (UCAS), Beijing 100049, China
| | - M Tacconi
- INFN Sezione di Milano-Bicocca, 20126 Milano, Italy
- Università di Milano-Bicocca, 20126 Milano, Italy
| | - X W Tang
- Institute of High Energy Physics (IHEP), Chinese Academy of Sciences, Beijing 100049, China
| | - Z C Tang
- Institute of High Energy Physics (IHEP), Chinese Academy of Sciences, Beijing 100049, China
| | - J Tian
- INFN Sezione di Roma Tor Vergata, 00133 Roma, Italy
| | - Y Tian
- Zhejiang University (ZJU), Hangzhou 310058, China
| | - Samuel C C Ting
- Massachusetts Institute of Technology (MIT), Cambridge, Massachusetts 02139, USA
- European Organization for Nuclear Research (CERN), 1211 Geneva 23, Switzerland
| | - S M Ting
- Massachusetts Institute of Technology (MIT), Cambridge, Massachusetts 02139, USA
| | - N Tomassetti
- INFN Sezione di Perugia, 06100 Perugia, Italy
- Università di Perugia, 06100 Perugia, Italy
| | - J Torsti
- Space Research Laboratory, Department of Physics and Astronomy, University of Turku, 20014 Turku, Finland
| | - T Urban
- Massachusetts Institute of Technology (MIT), Cambridge, Massachusetts 02139, USA
- National Aeronautics and Space Administration Johnson Space Center (JSC), Houston, Texas 77058, USA
| | - I Usoskin
- Sodankylä Geophysical Observatory and Space Physics and Astronomy Research Unit, University of Oulu, 90014 Oulu, Finland
| | - V Vagelli
- INFN Sezione di Perugia, 06100 Perugia, Italy
- Agenzia Spaziale Italiana (ASI), 00133 Roma, Italy
| | - R Vainio
- Space Research Laboratory, Department of Physics and Astronomy, University of Turku, 20014 Turku, Finland
| | - M Valencia-Otero
- Physics Department and Center for High Energy and High Field Physics, National Central University (NCU), Tao Yuan 32054, Taiwan
| | - E Valente
- INFN Sezione di Roma 1, 00185 Roma, Italy
- Università di Roma La Sapienza, 00185 Roma, Italy
| | - E Valtonen
- Space Research Laboratory, Department of Physics and Astronomy, University of Turku, 20014 Turku, Finland
| | - M Vázquez Acosta
- Instituto de Astrofísica de Canarias (IAC), 38205 La Laguna, and Departamento de Astrofísica, Universidad de La Laguna, 38206 La Laguna, Tenerife, Spain
| | - M Vecchi
- Kapteyn Astronomical Institute, University of Groningen, P.O. Box 800, 9700 AV Groningen, Netherlands
| | - M Velasco
- Centro de Investigaciones Energéticas, Medioambientales y Tecnológicas (CIEMAT), 28040 Madrid, Spain
| | - J P Vialle
- Université Grenoble Alpes, Université Savoie Mont Blanc, CNRS, LAPP-IN2P3, 74000 Annecy, France
| | - C X Wang
- Shandong University (SDU), Jinan, Shandong 250100, China
| | - L Wang
- Institute of Electrical Engineering (IEE), Chinese Academy of Sciences, Beijing 100190, China
| | - L Q Wang
- Shandong University (SDU), Jinan, Shandong 250100, China
| | - N H Wang
- Shandong University (SDU), Jinan, Shandong 250100, China
| | - Q L Wang
- Institute of Electrical Engineering (IEE), Chinese Academy of Sciences, Beijing 100190, China
| | - S Wang
- Physics and Astronomy Department, University of Hawaii, Honolulu, Hawaii 96822, USA
| | - X Wang
- Massachusetts Institute of Technology (MIT), Cambridge, Massachusetts 02139, USA
| | - Yu Wang
- Shandong University (SDU), Jinan, Shandong 250100, China
| | - Z M Wang
- Shandong Institute of Advanced Technology (SDIAT), Jinan, Shandong 250100, China
| | - J Wei
- DPNC, Université de Genève, 1211 Genève 4, Switzerland
- Shandong Institute of Advanced Technology (SDIAT), Jinan, Shandong 250100, China
| | - Z L Weng
- Massachusetts Institute of Technology (MIT), Cambridge, Massachusetts 02139, USA
| | - H Wu
- Southeast University (SEU), Nanjing 210096, China
| | - Y Wu
- Shandong Institute of Advanced Technology (SDIAT), Jinan, Shandong 250100, China
| | - J N Xiao
- Zhejiang University (ZJU), Hangzhou 310058, China
| | - R Q Xiong
- Southeast University (SEU), Nanjing 210096, China
| | - X Z Xiong
- Zhejiang University (ZJU), Hangzhou 310058, China
| | - W Xu
- Shandong University (SDU), Jinan, Shandong 250100, China
- Shandong Institute of Advanced Technology (SDIAT), Jinan, Shandong 250100, China
| | - Q Yan
- Massachusetts Institute of Technology (MIT), Cambridge, Massachusetts 02139, USA
| | - H T Yang
- Institute of High Energy Physics (IHEP), Chinese Academy of Sciences, Beijing 100049, China
- University of Chinese Academy of Sciences (UCAS), Beijing 100049, China
| | - Y Yang
- National Cheng Kung University, Tainan 70101, Taiwan
| | - I I Yashin
- NRNU MEPhI (Moscow Engineering Physics Institute), Moscow, 115409 Russia
| | - A Yelland
- Massachusetts Institute of Technology (MIT), Cambridge, Massachusetts 02139, USA
| | - H Yi
- Southeast University (SEU), Nanjing 210096, China
| | - Y H You
- Institute of High Energy Physics (IHEP), Chinese Academy of Sciences, Beijing 100049, China
- University of Chinese Academy of Sciences (UCAS), Beijing 100049, China
| | - Y M Yu
- Massachusetts Institute of Technology (MIT), Cambridge, Massachusetts 02139, USA
| | - Z Q Yu
- Institute of High Energy Physics (IHEP), Chinese Academy of Sciences, Beijing 100049, China
| | - M Zannoni
- INFN Sezione di Milano-Bicocca, 20126 Milano, Italy
- Università di Milano-Bicocca, 20126 Milano, Italy
| | - C Zhang
- Institute of High Energy Physics (IHEP), Chinese Academy of Sciences, Beijing 100049, China
| | - F Zhang
- Institute of High Energy Physics (IHEP), Chinese Academy of Sciences, Beijing 100049, China
| | - F Z Zhang
- Institute of High Energy Physics (IHEP), Chinese Academy of Sciences, Beijing 100049, China
- University of Chinese Academy of Sciences (UCAS), Beijing 100049, China
| | - J Zhang
- Shandong University (SDU), Jinan, Shandong 250100, China
| | - J H Zhang
- Southeast University (SEU), Nanjing 210096, China
| | - Z Zhang
- Massachusetts Institute of Technology (MIT), Cambridge, Massachusetts 02139, USA
| | - F Zhao
- Institute of High Energy Physics (IHEP), Chinese Academy of Sciences, Beijing 100049, China
- University of Chinese Academy of Sciences (UCAS), Beijing 100049, China
| | - C Zheng
- Shandong Institute of Advanced Technology (SDIAT), Jinan, Shandong 250100, China
| | - Z M Zheng
- Beihang University (BUAA), Beijing 100191, China
| | - H L Zhuang
- Institute of High Energy Physics (IHEP), Chinese Academy of Sciences, Beijing 100049, China
| | - V Zhukov
- I. Physics Institute and JARA-FAME, RWTH Aachen University, 52056 Aachen, Germany
| | - A Zichichi
- INFN Sezione di Bologna, 40126 Bologna, Italy
- Università di Bologna, 40126 Bologna, Italy
| | - P Zuccon
- INFN TIFPA, 38123 Trento, Italy
- Università di Trento, 38123 Trento, Italy
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6
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Krumholz MR, Crocker RM, Offner SSR. The cosmic ray ionization and γ-ray budgets of star-forming galaxies. MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY 2023; 520:5126-5143. [PMID: 36845327 PMCID: PMC9949718 DOI: 10.1093/mnras/stad459] [Citation(s) in RCA: 0] [Impact Index Per Article: 0] [Reference Citation Analysis] [Abstract] [Key Words] [Grants] [Track Full Text] [Subscribe] [Scholar Register] [Received: 11/07/2022] [Revised: 01/28/2023] [Accepted: 02/07/2023] [Indexed: 06/18/2023]
Abstract
Cosmic rays in star-forming galaxies are a dominant source of both diffuse γ-ray emission and ionization in gas too deeply shielded for photons to penetrate. Though the cosmic rays responsible for γ-rays and ionization are of different energies, they are produced by the same star formation-driven sources, and thus galaxies' star formation rates, γ-ray luminosities, and ionization rates should all be linked. In this paper, we use up-to-date cross-section data to determine this relationship, finding that cosmic rays in a galaxy of star formation rate [Formula: see text] and gas depletion time t dep produce a maximum primary ionization rate ζ ≈ 1 × 10-16(t dep/Gyr)-1 s-1 and a maximum γ-ray luminosity [Formula: see text] erg s-1 in the 0.1-100 GeV band. These budgets imply either that the ionization rates measured in Milky Way molecular clouds include a significant contribution from local sources that elevate them above the Galactic mean, or that CR-driven ionization in the Milky Way is enhanced by sources not linked directly to star formation. Our results also imply that ionization rates in starburst systems are only moderately enhanced compared to those in the Milky Way. Finally, we point out that measurements of γ-ray luminosities can be used to place constraints on galactic ionization budgets in starburst galaxies that are nearly free of systematic uncertainties on the details of cosmic ray acceleration.
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Affiliation(s)
- Mark R Krumholz
- Research School of Astronomy and Astrophysics, Australian National University, Canberra ACT 2600, Australia
- ARC Center of Excellence for Astronomy in Three Dimensions (ASTRO-3D), Canberra ACT 2600, Australia
| | - Roland M Crocker
- Research School of Astronomy and Astrophysics, Australian National University, Canberra ACT 2600, Australia
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7
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Tomassetti N, Bertucci B, Donnini F, Graziani M, Fiandrini E, Khiali B, Reina Conde A. Data driven analysis of cosmic rays in the heliosphere: diffusion of cosmic protons. RENDICONTI LINCEI. SCIENZE FISICHE E NATURALI 2023. [DOI: 10.1007/s12210-023-01149-1] [Citation(s) in RCA: 0] [Impact Index Per Article: 0] [Reference Citation Analysis] [Abstract] [Track Full Text] [Subscribe] [Scholar Register] [Indexed: 03/28/2023]
Abstract
AbstractUnderstanding the time-dependent relationship between the Sun’s variability and cosmic rays (GCR) is essential for developing predictive models of energetic radiation in space. When traveling inside the heliosphere, GCRs are affected by magnetic turbulence and solar wind disturbances which result in the so-called solar modulation effect. To investigate this phenomenon, we have performed a data-driven analysis of the temporal dependence of the GCR flux over the solar cycle. With a global statistical inference of GCR data collected in space by AMS-02 and PAMELA on monthly basis, we have determined the rigidity and time dependence of the GCR diffusion mean free path. Here we present our results for GCR protons, we discuss their interpretation in terms of basic processes of particle transport and their relations with the dynamics of the heliospheric plasma.
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8
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Brandt PC, Provornikova E, Bale SD, Cocoros A, DeMajistre R, Dialynas K, Elliott HA, Eriksson S, Fields B, Galli A, Hill ME, Horanyi M, Horbury T, Hunziker S, Kollmann P, Kinnison J, Fountain G, Krimigis SM, Kurth WS, Linsky J, Lisse CM, Mandt KE, Magnes W, McNutt RL, Miller J, Moebius E, Mostafavi P, Opher M, Paxton L, Plaschke F, Poppe AR, Roelof EC, Runyon K, Redfield S, Schwadron N, Sterken V, Swaczyna P, Szalay J, Turner D, Vannier H, Wimmer-Schweingruber R, Wurz P, Zirnstein EJ. Future Exploration of the Outer Heliosphere and Very Local Interstellar Medium by Interstellar Probe. SPACE SCIENCE REVIEWS 2023; 219:18. [PMID: 36874191 PMCID: PMC9974711 DOI: 10.1007/s11214-022-00943-x] [Citation(s) in RCA: 0] [Impact Index Per Article: 0] [Reference Citation Analysis] [Abstract] [Key Words] [Grants] [Track Full Text] [Figures] [Subscribe] [Scholar Register] [Received: 05/20/2022] [Accepted: 12/07/2022] [Indexed: 06/18/2023]
Abstract
A detailed overview of the knowledge gaps in our understanding of the heliospheric interaction with the largely unexplored Very Local Interstellar Medium (VLISM) are provided along with predictions of with the scientific discoveries that await. The new measurements required to make progress in this expanding frontier of space physics are discussed and include in-situ plasma and pick-up ion measurements throughout the heliosheath, direct sampling of the VLISM properties such as elemental and isotopic composition, densities, flows, and temperatures of neutral gas, dust and plasma, and remote energetic neutral atom (ENA) and Lyman-alpha (LYA) imaging from vantage points that can uniquely discern the heliospheric shape and bring new information on the interaction with interstellar hydrogen. The implementation of a pragmatic Interstellar Probe mission with a nominal design life to reach 375 Astronomical Units (au) with likely operation out to 550 au are reported as a result of a 4-year NASA funded mission study.
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Affiliation(s)
- P. C. Brandt
- The Johns Hopkins University Applied Physics Laboratory, Laurel, MD USA
| | - E. Provornikova
- The Johns Hopkins University Applied Physics Laboratory, Laurel, MD USA
| | - S. D. Bale
- University of California Berkeley, Berkeley, CA USA
| | - A. Cocoros
- The Johns Hopkins University Applied Physics Laboratory, Laurel, MD USA
| | - R. DeMajistre
- The Johns Hopkins University Applied Physics Laboratory, Laurel, MD USA
| | - K. Dialynas
- Office of Space Research and Technology, Academy of Athens, Athens, 10679 Greece
| | | | - S. Eriksson
- Laboratory for Atmospheric and Space Physics, University of Colorado at Boulder, Boulder, CO USA
| | - B. Fields
- University of Illinois Urbana-Champaign, Urbana, IL USA
| | - A. Galli
- University of Bern, Bern, Switzerland
| | - M. E. Hill
- The Johns Hopkins University Applied Physics Laboratory, Laurel, MD USA
| | - M. Horanyi
- Laboratory for Atmospheric and Space Physics, University of Colorado at Boulder, Boulder, CO USA
| | | | | | - P. Kollmann
- The Johns Hopkins University Applied Physics Laboratory, Laurel, MD USA
| | - J. Kinnison
- The Johns Hopkins University Applied Physics Laboratory, Laurel, MD USA
| | - G. Fountain
- The Johns Hopkins University Applied Physics Laboratory, Laurel, MD USA
| | - S. M. Krimigis
- Office of Space Research and Technology, Academy of Athens, Athens, 10679 Greece
| | | | - J. Linsky
- University of Colorado Boulder, Boulder, CO USA
| | - C. M. Lisse
- The Johns Hopkins University Applied Physics Laboratory, Laurel, MD USA
| | - K. E. Mandt
- The Johns Hopkins University Applied Physics Laboratory, Laurel, MD USA
| | - W. Magnes
- Space Research Institute, Austrian Academy of Sciences, Graz, Austria
| | - R. L. McNutt
- The Johns Hopkins University Applied Physics Laboratory, Laurel, MD USA
| | | | - E. Moebius
- University of New Hampshire, Durham, NH USA
| | - P. Mostafavi
- The Johns Hopkins University Applied Physics Laboratory, Laurel, MD USA
| | - M. Opher
- Boston University, Boston, MA USA
| | - L. Paxton
- The Johns Hopkins University Applied Physics Laboratory, Laurel, MD USA
| | - F. Plaschke
- Technical University Braunschweig, Braunschweig, Germany
| | - A. R. Poppe
- University of California Berkeley, Berkeley, CA USA
| | - E. C. Roelof
- The Johns Hopkins University Applied Physics Laboratory, Laurel, MD USA
| | - K. Runyon
- Planetary Science Institute, Tucson, AZ USA
| | | | | | | | | | - J. Szalay
- Princeton University, Princeton, NJ USA
| | - D. Turner
- The Johns Hopkins University Applied Physics Laboratory, Laurel, MD USA
| | | | | | - P. Wurz
- University of Bern, Bern, Switzerland
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9
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Abe K, Hayato Y, Hiraide K, Ieki K, Ikeda M, Kameda J, Kanemura Y, Kaneshima R, Kashiwagi Y, Kataoka Y, Miki S, Mine S, Miura M, Moriyama S, Nakano Y, Nakahata M, Nakayama S, Noguchi Y, Okamoto K, Sato K, Sekiya H, Shiba H, Shimizu K, Shiozawa M, Sonoda Y, Suzuki Y, Takeda A, Takemoto Y, Takenaka A, Tanaka H, Watanabe S, Yano T, Han S, Kajita T, Okumura K, Tashiro T, Tomiya T, Wang X, Xia J, Yoshida S, Megias GD, Fernandez P, Labarga L, Ospina N, Zaldivar B, Pointon BW, Kearns E, Raaf JL, Wan L, Wester T, Bian J, Griskevich NJ, Kropp WR, Locke S, Smy MB, Sobel HW, Takhistov V, Yankelevich A, Hill J, Park RG, Bodur B, Scholberg K, Walter CW, Bernard L, Coffani A, Drapier O, El Hedri S, Giampaolo A, Mueller TA, Santos AD, Paganini P, Quilain B, Ishizuka T, Nakamura T, Jang JS, Learned JG, Choi K, Cao S, Anthony LHV, Martin D, Scott M, Sztuc AA, Uchida Y, Berardi V, Catanesi MG, Radicioni E, Calabria NF, Machado LN, De Rosa G, Collazuol G, Iacob F, Lamoureux M, Mattiazzi M, Ludovici L, Gonin M, Pronost G, Fujisawa C, Maekawa Y, Nishimura Y, Friend M, Hasegawa T, Ishida T, Kobayashi T, Jakkapu M, Matsubara T, Nakadaira T, Nakamura K, Oyama Y, Sakashita K, Sekiguchi T, Tsukamoto T, Boschi T, Di Lodovico F, Gao J, Goldsack A, Katori T, Migenda J, Taani M, Zsoldos S, Kotsar Y, Ozaki H, Suzuki AT, Takeuchi Y, Bronner C, Feng J, Kikawa T, Mori M, Nakaya T, Wendell RA, Yasutome K, Jenkins SJ, McCauley N, Mehta P, Tsui KM, Fukuda Y, Itow Y, Menjo H, Ninomiya K, Lagoda J, Lakshmi SM, Mandal M, Mijakowski P, Prabhu YS, Zalipska J, Jia M, Jiang J, Jung CK, Wilking MJ, Yanagisawa C, Harada M, Ishino H, Ito S, Kitagawa H, Koshio Y, Nakanishi F, Sakai S, Barr G, Barrow D, Cook L, Samani S, Wark D, Nova F, Yang JY, Malek M, McElwee JM, Stone O, Thiesse MD, Thompson LF, Okazawa H, Kim SB, Seo JW, Yu I, Ichikawa AK, Nakamura KD, Tairafune S, Nishijima K, Iwamoto K, Nakagiri K, Nakajima Y, Taniuchi N, Yokoyama M, Martens K, de Perio P, Vagins MR, Kuze M, Izumiyama S, Inomoto M, Ishitsuka M, Ito H, Kinoshita T, Matsumoto R, Ommura Y, Shigeta N, Shinoki M, Suganuma T, Yamauchi K, Martin JF, Tanaka HA, Towstego T, Akutsu R, Gousy-Leblanc V, Hartz M, Konaka A, Prouse NW, Chen S, Xu BD, Zhang B, Posiadala-Zezula M, Hadley D, Nicholson M, O'Flaherty M, Richards B, Ali A, Jamieson B, Marti L, Minamino A, Pintaudi G, Sano S, Suzuki S, Wada K. Search for Cosmic-Ray Boosted Sub-GeV Dark Matter Using Recoil Protons at Super-Kamiokande. PHYSICAL REVIEW LETTERS 2023; 130:031802. [PMID: 36763398 DOI: 10.1103/physrevlett.130.031802] [Citation(s) in RCA: 0] [Impact Index Per Article: 0] [Reference Citation Analysis] [Abstract] [Grants] [Track Full Text] [Subscribe] [Scholar Register] [Received: 09/30/2022] [Accepted: 11/30/2022] [Indexed: 06/18/2023]
Abstract
We report a search for cosmic-ray boosted dark matter with protons using the 0.37 megaton×years data collected at Super-Kamiokande experiment during the 1996-2018 period (SKI-IV phase). We searched for an excess of proton recoils above the atmospheric neutrino background from the vicinity of the Galactic Center. No such excess is observed, and limits are calculated for two reference models of dark matter with either a constant interaction cross section or through a scalar mediator. This is the first experimental search for boosted dark matter with hadrons using directional information. The results present the most stringent limits on cosmic-ray boosted dark matter and exclude the dark matter-nucleon elastic scattering cross section between 10^{-33}cm^{2} and 10^{-27}cm^{2} for dark matter mass from 1 MeV/c^{2} to 300 MeV/c^{2}.
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Affiliation(s)
- K Abe
- Kamioka Observatory, Institute for Cosmic Ray Research, University of Tokyo, Kamioka, Gifu 506-1205, Japan
- Kavli Institute for the Physics and Mathematics of the Universe (WPI), The University of Tokyo Institutes for Advanced Study, University of Tokyo, Kashiwa, Chiba 277-8583, Japan
| | - Y Hayato
- Kamioka Observatory, Institute for Cosmic Ray Research, University of Tokyo, Kamioka, Gifu 506-1205, Japan
- Kavli Institute for the Physics and Mathematics of the Universe (WPI), The University of Tokyo Institutes for Advanced Study, University of Tokyo, Kashiwa, Chiba 277-8583, Japan
| | - K Hiraide
- Kamioka Observatory, Institute for Cosmic Ray Research, University of Tokyo, Kamioka, Gifu 506-1205, Japan
- Kavli Institute for the Physics and Mathematics of the Universe (WPI), The University of Tokyo Institutes for Advanced Study, University of Tokyo, Kashiwa, Chiba 277-8583, Japan
| | - K Ieki
- Kamioka Observatory, Institute for Cosmic Ray Research, University of Tokyo, Kamioka, Gifu 506-1205, Japan
- Kavli Institute for the Physics and Mathematics of the Universe (WPI), The University of Tokyo Institutes for Advanced Study, University of Tokyo, Kashiwa, Chiba 277-8583, Japan
| | - M Ikeda
- Kamioka Observatory, Institute for Cosmic Ray Research, University of Tokyo, Kamioka, Gifu 506-1205, Japan
- Kavli Institute for the Physics and Mathematics of the Universe (WPI), The University of Tokyo Institutes for Advanced Study, University of Tokyo, Kashiwa, Chiba 277-8583, Japan
| | - J Kameda
- Kamioka Observatory, Institute for Cosmic Ray Research, University of Tokyo, Kamioka, Gifu 506-1205, Japan
- Kavli Institute for the Physics and Mathematics of the Universe (WPI), The University of Tokyo Institutes for Advanced Study, University of Tokyo, Kashiwa, Chiba 277-8583, Japan
| | - Y Kanemura
- Kamioka Observatory, Institute for Cosmic Ray Research, University of Tokyo, Kamioka, Gifu 506-1205, Japan
| | - R Kaneshima
- Kamioka Observatory, Institute for Cosmic Ray Research, University of Tokyo, Kamioka, Gifu 506-1205, Japan
| | - Y Kashiwagi
- Kamioka Observatory, Institute for Cosmic Ray Research, University of Tokyo, Kamioka, Gifu 506-1205, Japan
| | - Y Kataoka
- Kamioka Observatory, Institute for Cosmic Ray Research, University of Tokyo, Kamioka, Gifu 506-1205, Japan
- Kavli Institute for the Physics and Mathematics of the Universe (WPI), The University of Tokyo Institutes for Advanced Study, University of Tokyo, Kashiwa, Chiba 277-8583, Japan
| | - S Miki
- Kamioka Observatory, Institute for Cosmic Ray Research, University of Tokyo, Kamioka, Gifu 506-1205, Japan
| | - S Mine
- Kamioka Observatory, Institute for Cosmic Ray Research, University of Tokyo, Kamioka, Gifu 506-1205, Japan
- Department of Physics and Astronomy, University of California, Irvine, Irvine, California 92697-4575, USA
| | - M Miura
- Kamioka Observatory, Institute for Cosmic Ray Research, University of Tokyo, Kamioka, Gifu 506-1205, Japan
- Kavli Institute for the Physics and Mathematics of the Universe (WPI), The University of Tokyo Institutes for Advanced Study, University of Tokyo, Kashiwa, Chiba 277-8583, Japan
| | - S Moriyama
- Kamioka Observatory, Institute for Cosmic Ray Research, University of Tokyo, Kamioka, Gifu 506-1205, Japan
- Kavli Institute for the Physics and Mathematics of the Universe (WPI), The University of Tokyo Institutes for Advanced Study, University of Tokyo, Kashiwa, Chiba 277-8583, Japan
| | - Y Nakano
- Kamioka Observatory, Institute for Cosmic Ray Research, University of Tokyo, Kamioka, Gifu 506-1205, Japan
| | - M Nakahata
- Kamioka Observatory, Institute for Cosmic Ray Research, University of Tokyo, Kamioka, Gifu 506-1205, Japan
- Kavli Institute for the Physics and Mathematics of the Universe (WPI), The University of Tokyo Institutes for Advanced Study, University of Tokyo, Kashiwa, Chiba 277-8583, Japan
| | - S Nakayama
- Kamioka Observatory, Institute for Cosmic Ray Research, University of Tokyo, Kamioka, Gifu 506-1205, Japan
- Kavli Institute for the Physics and Mathematics of the Universe (WPI), The University of Tokyo Institutes for Advanced Study, University of Tokyo, Kashiwa, Chiba 277-8583, Japan
| | - Y Noguchi
- Kamioka Observatory, Institute for Cosmic Ray Research, University of Tokyo, Kamioka, Gifu 506-1205, Japan
| | - K Okamoto
- Kamioka Observatory, Institute for Cosmic Ray Research, University of Tokyo, Kamioka, Gifu 506-1205, Japan
| | - K Sato
- Kamioka Observatory, Institute for Cosmic Ray Research, University of Tokyo, Kamioka, Gifu 506-1205, Japan
| | - H Sekiya
- Kamioka Observatory, Institute for Cosmic Ray Research, University of Tokyo, Kamioka, Gifu 506-1205, Japan
- Kavli Institute for the Physics and Mathematics of the Universe (WPI), The University of Tokyo Institutes for Advanced Study, University of Tokyo, Kashiwa, Chiba 277-8583, Japan
| | - H Shiba
- Kamioka Observatory, Institute for Cosmic Ray Research, University of Tokyo, Kamioka, Gifu 506-1205, Japan
| | - K Shimizu
- Kamioka Observatory, Institute for Cosmic Ray Research, University of Tokyo, Kamioka, Gifu 506-1205, Japan
| | - M Shiozawa
- Kamioka Observatory, Institute for Cosmic Ray Research, University of Tokyo, Kamioka, Gifu 506-1205, Japan
- Kavli Institute for the Physics and Mathematics of the Universe (WPI), The University of Tokyo Institutes for Advanced Study, University of Tokyo, Kashiwa, Chiba 277-8583, Japan
| | - Y Sonoda
- Kamioka Observatory, Institute for Cosmic Ray Research, University of Tokyo, Kamioka, Gifu 506-1205, Japan
| | - Y Suzuki
- Kamioka Observatory, Institute for Cosmic Ray Research, University of Tokyo, Kamioka, Gifu 506-1205, Japan
| | - A Takeda
- Kamioka Observatory, Institute for Cosmic Ray Research, University of Tokyo, Kamioka, Gifu 506-1205, Japan
- Kavli Institute for the Physics and Mathematics of the Universe (WPI), The University of Tokyo Institutes for Advanced Study, University of Tokyo, Kashiwa, Chiba 277-8583, Japan
| | - Y Takemoto
- Kamioka Observatory, Institute for Cosmic Ray Research, University of Tokyo, Kamioka, Gifu 506-1205, Japan
- Kavli Institute for the Physics and Mathematics of the Universe (WPI), The University of Tokyo Institutes for Advanced Study, University of Tokyo, Kashiwa, Chiba 277-8583, Japan
| | - A Takenaka
- Kamioka Observatory, Institute for Cosmic Ray Research, University of Tokyo, Kamioka, Gifu 506-1205, Japan
| | - H Tanaka
- Kamioka Observatory, Institute for Cosmic Ray Research, University of Tokyo, Kamioka, Gifu 506-1205, Japan
- Kavli Institute for the Physics and Mathematics of the Universe (WPI), The University of Tokyo Institutes for Advanced Study, University of Tokyo, Kashiwa, Chiba 277-8583, Japan
| | - S Watanabe
- Kamioka Observatory, Institute for Cosmic Ray Research, University of Tokyo, Kamioka, Gifu 506-1205, Japan
| | - T Yano
- Kamioka Observatory, Institute for Cosmic Ray Research, University of Tokyo, Kamioka, Gifu 506-1205, Japan
| | - S Han
- Research Center for Cosmic Neutrinos, Institute for Cosmic Ray Research, University of Tokyo, Kashiwa, Chiba 277-8582, Japan
| | - T Kajita
- Research Center for Cosmic Neutrinos, Institute for Cosmic Ray Research, University of Tokyo, Kashiwa, Chiba 277-8582, Japan
- ILANCE, CNRS-University of Tokyo International Research Laboratory, Kashiwa, Chiba 277-8582, Japan
- Kavli Institute for the Physics and Mathematics of the Universe (WPI), The University of Tokyo Institutes for Advanced Study, University of Tokyo, Kashiwa, Chiba 277-8583, Japan
| | - K Okumura
- Research Center for Cosmic Neutrinos, Institute for Cosmic Ray Research, University of Tokyo, Kashiwa, Chiba 277-8582, Japan
- Kavli Institute for the Physics and Mathematics of the Universe (WPI), The University of Tokyo Institutes for Advanced Study, University of Tokyo, Kashiwa, Chiba 277-8583, Japan
| | - T Tashiro
- Research Center for Cosmic Neutrinos, Institute for Cosmic Ray Research, University of Tokyo, Kashiwa, Chiba 277-8582, Japan
| | - T Tomiya
- Research Center for Cosmic Neutrinos, Institute for Cosmic Ray Research, University of Tokyo, Kashiwa, Chiba 277-8582, Japan
| | - X Wang
- Research Center for Cosmic Neutrinos, Institute for Cosmic Ray Research, University of Tokyo, Kashiwa, Chiba 277-8582, Japan
| | - J Xia
- Research Center for Cosmic Neutrinos, Institute for Cosmic Ray Research, University of Tokyo, Kashiwa, Chiba 277-8582, Japan
| | - S Yoshida
- Research Center for Cosmic Neutrinos, Institute for Cosmic Ray Research, University of Tokyo, Kashiwa, Chiba 277-8582, Japan
| | - G D Megias
- Institute for Cosmic Ray Research, University of Tokyo, Kashiwa, Chiba 277-8582, Japan
| | - P Fernandez
- Department of Theoretical Physics, University Autonoma Madrid, 28049 Madrid, Spain
| | - L Labarga
- Department of Theoretical Physics, University Autonoma Madrid, 28049 Madrid, Spain
| | - N Ospina
- Department of Theoretical Physics, University Autonoma Madrid, 28049 Madrid, Spain
| | - B Zaldivar
- Department of Theoretical Physics, University Autonoma Madrid, 28049 Madrid, Spain
| | - B W Pointon
- Department of Physics, British Columbia Institute of Technology, Burnaby, British Columbia V5G 3H2, Canada
- TRIUMF, 4004 Wesbrook Mall, Vancouver, British Columbia V6T2A3, Canada
| | - E Kearns
- Department of Physics, Boston University, Boston, Massachusetts 02215, USA
- Kavli Institute for the Physics and Mathematics of the Universe (WPI), The University of Tokyo Institutes for Advanced Study, University of Tokyo, Kashiwa, Chiba 277-8583, Japan
| | - J L Raaf
- Department of Physics, Boston University, Boston, Massachusetts 02215, USA
| | - L Wan
- Department of Physics, Boston University, Boston, Massachusetts 02215, USA
| | - T Wester
- Department of Physics, Boston University, Boston, Massachusetts 02215, USA
| | - J Bian
- Department of Physics and Astronomy, University of California, Irvine, Irvine, California 92697-4575, USA
| | - N J Griskevich
- Department of Physics and Astronomy, University of California, Irvine, Irvine, California 92697-4575, USA
| | - W R Kropp
- Department of Physics and Astronomy, University of California, Irvine, Irvine, California 92697-4575, USA
| | - S Locke
- Department of Physics and Astronomy, University of California, Irvine, Irvine, California 92697-4575, USA
| | - M B Smy
- Department of Physics and Astronomy, University of California, Irvine, Irvine, California 92697-4575, USA
- Kavli Institute for the Physics and Mathematics of the Universe (WPI), The University of Tokyo Institutes for Advanced Study, University of Tokyo, Kashiwa, Chiba 277-8583, Japan
| | - H W Sobel
- Department of Physics and Astronomy, University of California, Irvine, Irvine, California 92697-4575, USA
- Kavli Institute for the Physics and Mathematics of the Universe (WPI), The University of Tokyo Institutes for Advanced Study, University of Tokyo, Kashiwa, Chiba 277-8583, Japan
| | - V Takhistov
- Department of Physics and Astronomy, University of California, Irvine, Irvine, California 92697-4575, USA
- High Energy Accelerator Research Organization (KEK), Tsukuba, Ibaraki 305-0801, Japan
- Kavli Institute for the Physics and Mathematics of the Universe (WPI), The University of Tokyo Institutes for Advanced Study, University of Tokyo, Kashiwa, Chiba 277-8583, Japan
| | - A Yankelevich
- Department of Physics and Astronomy, University of California, Irvine, Irvine, California 92697-4575, USA
| | - J Hill
- Department of Physics, California State University, Dominguez Hills, Carson, California 90747, USA
| | - R G Park
- Institute for Universe and Elementary Particles, Chonnam National University, Gwangju 61186, Korea
| | - B Bodur
- Department of Physics, Duke University, Durham, North Carolina 27708, USA
| | - K Scholberg
- Department of Physics, Duke University, Durham, North Carolina 27708, USA
- Kavli Institute for the Physics and Mathematics of the Universe (WPI), The University of Tokyo Institutes for Advanced Study, University of Tokyo, Kashiwa, Chiba 277-8583, Japan
| | - C W Walter
- Department of Physics, Duke University, Durham, North Carolina 27708, USA
- Kavli Institute for the Physics and Mathematics of the Universe (WPI), The University of Tokyo Institutes for Advanced Study, University of Tokyo, Kashiwa, Chiba 277-8583, Japan
| | - L Bernard
- Ecole Polytechnique, IN2P3-CNRS, Laboratoire Leprince-Ringuet, F-91120 Palaiseau, France
| | - A Coffani
- Ecole Polytechnique, IN2P3-CNRS, Laboratoire Leprince-Ringuet, F-91120 Palaiseau, France
| | - O Drapier
- Ecole Polytechnique, IN2P3-CNRS, Laboratoire Leprince-Ringuet, F-91120 Palaiseau, France
| | - S El Hedri
- Ecole Polytechnique, IN2P3-CNRS, Laboratoire Leprince-Ringuet, F-91120 Palaiseau, France
| | - A Giampaolo
- Ecole Polytechnique, IN2P3-CNRS, Laboratoire Leprince-Ringuet, F-91120 Palaiseau, France
| | - Th A Mueller
- Ecole Polytechnique, IN2P3-CNRS, Laboratoire Leprince-Ringuet, F-91120 Palaiseau, France
| | - A D Santos
- Ecole Polytechnique, IN2P3-CNRS, Laboratoire Leprince-Ringuet, F-91120 Palaiseau, France
| | - P Paganini
- Ecole Polytechnique, IN2P3-CNRS, Laboratoire Leprince-Ringuet, F-91120 Palaiseau, France
| | - B Quilain
- Ecole Polytechnique, IN2P3-CNRS, Laboratoire Leprince-Ringuet, F-91120 Palaiseau, France
| | - T Ishizuka
- Junior College, Fukuoka Institute of Technology, Fukuoka, Fukuoka 811-0295, Japan
| | - T Nakamura
- Department of Physics, Gifu University, Gifu, Gifu 501-1193, Japan
| | - J S Jang
- GIST College, Gwangju Institute of Science and Technology, Gwangju 500-712, Korea
| | - J G Learned
- Department of Physics and Astronomy, University of Hawaii, Honolulu, Hawaii 96822, USA
| | - K Choi
- Institute for Basic Science (IBS), Daejeon 34126, Korea
| | - S Cao
- Institute For Interdisciplinary Research in Science and Education, ICISE, Quy Nhon 55121, Vietnam
| | - L H V Anthony
- Department of Physics, Imperial College London, London SW7 2AZ, United Kingdom
| | - D Martin
- Department of Physics, Imperial College London, London SW7 2AZ, United Kingdom
| | - M Scott
- Department of Physics, Imperial College London, London SW7 2AZ, United Kingdom
| | - A A Sztuc
- Department of Physics, Imperial College London, London SW7 2AZ, United Kingdom
| | - Y Uchida
- Department of Physics, Imperial College London, London SW7 2AZ, United Kingdom
| | - V Berardi
- Dipartimento Interuniversitario di Fisica, INFN Sezione di Bari and Università e Politecnico di Bari, I-70125 Bari, Italy
| | - M G Catanesi
- Dipartimento Interuniversitario di Fisica, INFN Sezione di Bari and Università e Politecnico di Bari, I-70125 Bari, Italy
| | - E Radicioni
- Dipartimento Interuniversitario di Fisica, INFN Sezione di Bari and Università e Politecnico di Bari, I-70125 Bari, Italy
| | - N F Calabria
- Dipartimento di Fisica, INFN Sezione di Napoli and Università di Napoli, I-80126 Napoli, Italy
| | - L N Machado
- Dipartimento di Fisica, INFN Sezione di Napoli and Università di Napoli, I-80126 Napoli, Italy
| | - G De Rosa
- Dipartimento di Fisica, INFN Sezione di Napoli and Università di Napoli, I-80126 Napoli, Italy
| | - G Collazuol
- Dipartimento di Fisica, INFN Sezione di Padova and Università di Padova, I-35131 Padova, Italy
| | - F Iacob
- Dipartimento di Fisica, INFN Sezione di Padova and Università di Padova, I-35131 Padova, Italy
| | - M Lamoureux
- Dipartimento di Fisica, INFN Sezione di Padova and Università di Padova, I-35131 Padova, Italy
| | - M Mattiazzi
- Dipartimento di Fisica, INFN Sezione di Padova and Università di Padova, I-35131 Padova, Italy
| | - L Ludovici
- INFN Sezione di Roma and Università di Roma "La Sapienza," I-00185, Roma, Italy
| | - M Gonin
- ILANCE, CNRS-University of Tokyo International Research Laboratory, Kashiwa, Chiba 277-8582, Japan
| | - G Pronost
- ILANCE, CNRS-University of Tokyo International Research Laboratory, Kashiwa, Chiba 277-8582, Japan
| | - C Fujisawa
- Department of Physics, Keio University, Yokohama, Kanagawa 223-8522, Japan
| | - Y Maekawa
- Department of Physics, Keio University, Yokohama, Kanagawa 223-8522, Japan
| | - Y Nishimura
- Department of Physics, Keio University, Yokohama, Kanagawa 223-8522, Japan
| | - M Friend
- High Energy Accelerator Research Organization (KEK), Tsukuba, Ibaraki 305-0801, Japan
| | - T Hasegawa
- High Energy Accelerator Research Organization (KEK), Tsukuba, Ibaraki 305-0801, Japan
| | - T Ishida
- High Energy Accelerator Research Organization (KEK), Tsukuba, Ibaraki 305-0801, Japan
| | - T Kobayashi
- High Energy Accelerator Research Organization (KEK), Tsukuba, Ibaraki 305-0801, Japan
| | - M Jakkapu
- High Energy Accelerator Research Organization (KEK), Tsukuba, Ibaraki 305-0801, Japan
| | - T Matsubara
- High Energy Accelerator Research Organization (KEK), Tsukuba, Ibaraki 305-0801, Japan
| | - T Nakadaira
- High Energy Accelerator Research Organization (KEK), Tsukuba, Ibaraki 305-0801, Japan
| | - K Nakamura
- High Energy Accelerator Research Organization (KEK), Tsukuba, Ibaraki 305-0801, Japan
- Kavli Institute for the Physics and Mathematics of the Universe (WPI), The University of Tokyo Institutes for Advanced Study, University of Tokyo, Kashiwa, Chiba 277-8583, Japan
| | - Y Oyama
- High Energy Accelerator Research Organization (KEK), Tsukuba, Ibaraki 305-0801, Japan
| | - K Sakashita
- High Energy Accelerator Research Organization (KEK), Tsukuba, Ibaraki 305-0801, Japan
| | - T Sekiguchi
- High Energy Accelerator Research Organization (KEK), Tsukuba, Ibaraki 305-0801, Japan
| | - T Tsukamoto
- High Energy Accelerator Research Organization (KEK), Tsukuba, Ibaraki 305-0801, Japan
| | - T Boschi
- Department of Physics, King's College London, London WC2R 2LS, United Kingdom
| | - F Di Lodovico
- Department of Physics, King's College London, London WC2R 2LS, United Kingdom
| | - J Gao
- Department of Physics, King's College London, London WC2R 2LS, United Kingdom
| | - A Goldsack
- Department of Physics, King's College London, London WC2R 2LS, United Kingdom
| | - T Katori
- Department of Physics, King's College London, London WC2R 2LS, United Kingdom
| | - J Migenda
- Department of Physics, King's College London, London WC2R 2LS, United Kingdom
| | - M Taani
- Department of Physics, King's College London, London WC2R 2LS, United Kingdom
| | - S Zsoldos
- Department of Physics, King's College London, London WC2R 2LS, United Kingdom
- Kavli Institute for the Physics and Mathematics of the Universe (WPI), The University of Tokyo Institutes for Advanced Study, University of Tokyo, Kashiwa, Chiba 277-8583, Japan
| | - Y Kotsar
- Department of Physics, Kobe University, Kobe, Hyogo 657-8501, Japan
| | - H Ozaki
- Department of Physics, Kobe University, Kobe, Hyogo 657-8501, Japan
| | - A T Suzuki
- Department of Physics, Kobe University, Kobe, Hyogo 657-8501, Japan
| | - Y Takeuchi
- Department of Physics, Kobe University, Kobe, Hyogo 657-8501, Japan
- Kavli Institute for the Physics and Mathematics of the Universe (WPI), The University of Tokyo Institutes for Advanced Study, University of Tokyo, Kashiwa, Chiba 277-8583, Japan
| | - C Bronner
- Department of Physics, Kyoto University, Kyoto, Kyoto 606-8502, Japan
| | - J Feng
- Department of Physics, Kyoto University, Kyoto, Kyoto 606-8502, Japan
| | - T Kikawa
- Department of Physics, Kyoto University, Kyoto, Kyoto 606-8502, Japan
| | - M Mori
- Department of Physics, Kyoto University, Kyoto, Kyoto 606-8502, Japan
| | - T Nakaya
- Department of Physics, Kyoto University, Kyoto, Kyoto 606-8502, Japan
- Kavli Institute for the Physics and Mathematics of the Universe (WPI), The University of Tokyo Institutes for Advanced Study, University of Tokyo, Kashiwa, Chiba 277-8583, Japan
| | - R A Wendell
- Department of Physics, Kyoto University, Kyoto, Kyoto 606-8502, Japan
- Kavli Institute for the Physics and Mathematics of the Universe (WPI), The University of Tokyo Institutes for Advanced Study, University of Tokyo, Kashiwa, Chiba 277-8583, Japan
| | - K Yasutome
- Department of Physics, Kyoto University, Kyoto, Kyoto 606-8502, Japan
| | - S J Jenkins
- Department of Physics, University of Liverpool, Liverpool L69 7ZE, United Kingdom
| | - N McCauley
- Department of Physics, University of Liverpool, Liverpool L69 7ZE, United Kingdom
| | - P Mehta
- Department of Physics, University of Liverpool, Liverpool L69 7ZE, United Kingdom
| | - K M Tsui
- Department of Physics, University of Liverpool, Liverpool L69 7ZE, United Kingdom
| | - Y Fukuda
- Department of Physics, Miyagi University of Education, Sendai, Miyagi 980-0845, Japan
| | - Y Itow
- Institute for Space-Earth Environmental Research, Nagoya University, Nagoya, Aichi 464-8602, Japan
- Kobayashi-Maskawa Institute for the Origin of Particles and the Universe, Nagoya University, Nagoya, Aichi 464-8602, Japan
| | - H Menjo
- Institute for Space-Earth Environmental Research, Nagoya University, Nagoya, Aichi 464-8602, Japan
| | - K Ninomiya
- Institute for Space-Earth Environmental Research, Nagoya University, Nagoya, Aichi 464-8602, Japan
| | - J Lagoda
- National Centre For Nuclear Research, 02-093 Warsaw, Poland
| | - S M Lakshmi
- National Centre For Nuclear Research, 02-093 Warsaw, Poland
| | - M Mandal
- National Centre For Nuclear Research, 02-093 Warsaw, Poland
| | - P Mijakowski
- National Centre For Nuclear Research, 02-093 Warsaw, Poland
| | - Y S Prabhu
- National Centre For Nuclear Research, 02-093 Warsaw, Poland
| | - J Zalipska
- National Centre For Nuclear Research, 02-093 Warsaw, Poland
| | - M Jia
- Department of Physics and Astronomy, State University of New York at Stony Brook, New York 11794-3800, USA
| | - J Jiang
- Department of Physics and Astronomy, State University of New York at Stony Brook, New York 11794-3800, USA
| | - C K Jung
- Department of Physics and Astronomy, State University of New York at Stony Brook, New York 11794-3800, USA
| | - M J Wilking
- Department of Physics and Astronomy, State University of New York at Stony Brook, New York 11794-3800, USA
| | - C Yanagisawa
- Department of Physics and Astronomy, State University of New York at Stony Brook, New York 11794-3800, USA
| | - M Harada
- Department of Physics, Okayama University, Okayama, Okayama 700-8530, Japan
| | - H Ishino
- Department of Physics, Okayama University, Okayama, Okayama 700-8530, Japan
| | - S Ito
- Department of Physics, Okayama University, Okayama, Okayama 700-8530, Japan
| | - H Kitagawa
- Department of Physics, Okayama University, Okayama, Okayama 700-8530, Japan
| | - Y Koshio
- Department of Physics, Okayama University, Okayama, Okayama 700-8530, Japan
- Kavli Institute for the Physics and Mathematics of the Universe (WPI), The University of Tokyo Institutes for Advanced Study, University of Tokyo, Kashiwa, Chiba 277-8583, Japan
| | - F Nakanishi
- Department of Physics, Okayama University, Okayama, Okayama 700-8530, Japan
| | - S Sakai
- Department of Physics, Okayama University, Okayama, Okayama 700-8530, Japan
| | - G Barr
- Department of Physics, Oxford University, Oxford OX1 3PU, United Kingdom
| | - D Barrow
- Department of Physics, Oxford University, Oxford OX1 3PU, United Kingdom
| | - L Cook
- Department of Physics, Oxford University, Oxford OX1 3PU, United Kingdom
- Kavli Institute for the Physics and Mathematics of the Universe (WPI), The University of Tokyo Institutes for Advanced Study, University of Tokyo, Kashiwa, Chiba 277-8583, Japan
| | - S Samani
- Department of Physics, Oxford University, Oxford OX1 3PU, United Kingdom
| | - D Wark
- Department of Physics, Oxford University, Oxford OX1 3PU, United Kingdom
- STFC, Rutherford Appleton Laboratory, Harwell Oxford, and Daresbury Laboratory, Warrington OX11 0QX, United Kingdom
| | - F Nova
- Rutherford Appleton Laboratory, Harwell, Oxford OX11 0QX, United Kingdom
| | - J Y Yang
- Department of Physics, Seoul National University, Seoul 151-742, Korea
| | - M Malek
- Department of Physics and Astronomy, University of Sheffield, S3 7RH Sheffield, United Kingdom
| | - J M McElwee
- Department of Physics and Astronomy, University of Sheffield, S3 7RH Sheffield, United Kingdom
| | - O Stone
- Department of Physics and Astronomy, University of Sheffield, S3 7RH Sheffield, United Kingdom
| | - M D Thiesse
- Department of Physics and Astronomy, University of Sheffield, S3 7RH Sheffield, United Kingdom
| | - L F Thompson
- Department of Physics and Astronomy, University of Sheffield, S3 7RH Sheffield, United Kingdom
| | - H Okazawa
- Department of Informatics in Social Welfare, Shizuoka University of Welfare, Yaizu, Shizuoka 425-8611, Japan
| | - S B Kim
- Department of Physics, Sungkyunkwan University, Suwon 440-746, Korea
| | - J W Seo
- Department of Physics, Sungkyunkwan University, Suwon 440-746, Korea
| | - I Yu
- Department of Physics, Sungkyunkwan University, Suwon 440-746, Korea
| | - A K Ichikawa
- Department of Physics, Faculty of Science, Tohoku University, Sendai, Miyagi 980-8578, Japan
| | - K D Nakamura
- Department of Physics, Faculty of Science, Tohoku University, Sendai, Miyagi 980-8578, Japan
| | - S Tairafune
- Department of Physics, Faculty of Science, Tohoku University, Sendai, Miyagi 980-8578, Japan
| | - K Nishijima
- Department of Physics, Tokai University, Hiratsuka, Kanagawa 259-1292, Japan
| | - K Iwamoto
- Department of Physics, University of Tokyo, Bunkyo, Tokyo 113-0033, Japan
| | - K Nakagiri
- Department of Physics, University of Tokyo, Bunkyo, Tokyo 113-0033, Japan
| | - Y Nakajima
- Department of Physics, University of Tokyo, Bunkyo, Tokyo 113-0033, Japan
- Kavli Institute for the Physics and Mathematics of the Universe (WPI), The University of Tokyo Institutes for Advanced Study, University of Tokyo, Kashiwa, Chiba 277-8583, Japan
| | - N Taniuchi
- Department of Physics, University of Tokyo, Bunkyo, Tokyo 113-0033, Japan
| | - M Yokoyama
- Department of Physics, University of Tokyo, Bunkyo, Tokyo 113-0033, Japan
- Kavli Institute for the Physics and Mathematics of the Universe (WPI), The University of Tokyo Institutes for Advanced Study, University of Tokyo, Kashiwa, Chiba 277-8583, Japan
| | - K Martens
- Kavli Institute for the Physics and Mathematics of the Universe (WPI), The University of Tokyo Institutes for Advanced Study, University of Tokyo, Kashiwa, Chiba 277-8583, Japan
| | - P de Perio
- Kavli Institute for the Physics and Mathematics of the Universe (WPI), The University of Tokyo Institutes for Advanced Study, University of Tokyo, Kashiwa, Chiba 277-8583, Japan
| | - M R Vagins
- Department of Physics and Astronomy, University of California, Irvine, Irvine, California 92697-4575, USA
- Kavli Institute for the Physics and Mathematics of the Universe (WPI), The University of Tokyo Institutes for Advanced Study, University of Tokyo, Kashiwa, Chiba 277-8583, Japan
| | - M Kuze
- Department of Physics, Tokyo Institute of Technology, Meguro, Tokyo 152-8551, Japan
| | - S Izumiyama
- Department of Physics, Tokyo Institute of Technology, Meguro, Tokyo 152-8551, Japan
| | - M Inomoto
- Department of Physics, Faculty of Science and Technology, Tokyo University of Science, Noda, Chiba 278-8510, Japan
| | - M Ishitsuka
- Department of Physics, Faculty of Science and Technology, Tokyo University of Science, Noda, Chiba 278-8510, Japan
| | - H Ito
- Department of Physics, Faculty of Science and Technology, Tokyo University of Science, Noda, Chiba 278-8510, Japan
| | - T Kinoshita
- Department of Physics, Faculty of Science and Technology, Tokyo University of Science, Noda, Chiba 278-8510, Japan
| | - R Matsumoto
- Department of Physics, Faculty of Science and Technology, Tokyo University of Science, Noda, Chiba 278-8510, Japan
| | - Y Ommura
- Department of Physics, Faculty of Science and Technology, Tokyo University of Science, Noda, Chiba 278-8510, Japan
| | - N Shigeta
- Department of Physics, Faculty of Science and Technology, Tokyo University of Science, Noda, Chiba 278-8510, Japan
| | - M Shinoki
- Department of Physics, Faculty of Science and Technology, Tokyo University of Science, Noda, Chiba 278-8510, Japan
| | - T Suganuma
- Department of Physics, Faculty of Science and Technology, Tokyo University of Science, Noda, Chiba 278-8510, Japan
| | - K Yamauchi
- Department of Physics, Faculty of Science and Technology, Tokyo University of Science, Noda, Chiba 278-8510, Japan
| | - J F Martin
- Department of Physics, University of Toronto, Ontario M5S 1A7, Canada
| | - H A Tanaka
- Department of Physics, University of Toronto, Ontario M5S 1A7, Canada
| | - T Towstego
- Department of Physics, University of Toronto, Ontario M5S 1A7, Canada
| | - R Akutsu
- TRIUMF, 4004 Wesbrook Mall, Vancouver, British Columbia V6T2A3, Canada
| | - V Gousy-Leblanc
- TRIUMF, 4004 Wesbrook Mall, Vancouver, British Columbia V6T2A3, Canada
| | - M Hartz
- TRIUMF, 4004 Wesbrook Mall, Vancouver, British Columbia V6T2A3, Canada
| | - A Konaka
- TRIUMF, 4004 Wesbrook Mall, Vancouver, British Columbia V6T2A3, Canada
| | - N W Prouse
- TRIUMF, 4004 Wesbrook Mall, Vancouver, British Columbia V6T2A3, Canada
| | - S Chen
- Department of Engineering Physics, Tsinghua University, Beijing, 100084, China
| | - B D Xu
- Department of Engineering Physics, Tsinghua University, Beijing, 100084, China
| | - B Zhang
- Department of Engineering Physics, Tsinghua University, Beijing, 100084, China
| | | | - D Hadley
- Department of Physics, University of Warwick, Coventry, CV4 7AL, United Kingdom
| | - M Nicholson
- Department of Physics, University of Warwick, Coventry, CV4 7AL, United Kingdom
| | - M O'Flaherty
- Department of Physics, University of Warwick, Coventry, CV4 7AL, United Kingdom
| | - B Richards
- Department of Physics, University of Warwick, Coventry, CV4 7AL, United Kingdom
| | - A Ali
- TRIUMF, 4004 Wesbrook Mall, Vancouver, British Columbia V6T2A3, Canada
- Department of Physics, University of Winnipeg, Manitoba R3J 3L8, Canada
| | - B Jamieson
- Department of Physics, University of Winnipeg, Manitoba R3J 3L8, Canada
| | - Ll Marti
- Department of Physics, Yokohama National University, Yokohama, Kanagawa 240-8501, Japan
| | - A Minamino
- Department of Physics, Yokohama National University, Yokohama, Kanagawa 240-8501, Japan
| | - G Pintaudi
- Department of Physics, Yokohama National University, Yokohama, Kanagawa 240-8501, Japan
| | - S Sano
- Department of Physics, Yokohama National University, Yokohama, Kanagawa 240-8501, Japan
| | - S Suzuki
- Department of Physics, Yokohama National University, Yokohama, Kanagawa 240-8501, Japan
| | - K Wada
- Department of Physics, Yokohama National University, Yokohama, Kanagawa 240-8501, Japan
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10
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Zhu CR, Cui MY, Xia ZQ, Yu ZH, Huang X, Yuan Q, Fan YZ. Explaining the GeV Antiproton Excess, GeV γ-Ray Excess, and W-Boson Mass Anomaly in an Inert Two Higgs Doublet Model. PHYSICAL REVIEW LETTERS 2022; 129:231101. [PMID: 36563204 DOI: 10.1103/physrevlett.129.231101] [Citation(s) in RCA: 0] [Impact Index Per Article: 0] [Reference Citation Analysis] [Abstract] [Track Full Text] [Subscribe] [Scholar Register] [Received: 04/15/2022] [Revised: 09/20/2022] [Accepted: 10/31/2022] [Indexed: 06/17/2023]
Abstract
For the newly discovered W-boson mass anomaly, one of the simplest dark matter (DM) models that can account for the anomaly without violating other astrophysical and experimental constraints is the inert two Higgs doublet model, in which the DM mass (m_{S}) is found to be within ∼54-74 GeV. In this model, the annihilation of DM via SS→bb[over ¯] and SS→WW^{*} would produce antiprotons and gamma rays, and may account for the excesses identified previously in both particles. Motivated by this, we reanalyze the AMS-02 antiproton and Fermi-LAT Galactic center γ-ray data. For the antiproton analysis, the novel treatment is the inclusion of the charge-sign-dependent three-dimensional solar modulation model as constrained by the time-dependent proton data. We find that the excess of antiprotons is more distinct than previous results based on the force-field solar modulation model. The interpretation of this excess as the annihilation of SS→WW^{*} (SS→bb[over ¯]) requires a DM mass of ∼40-80 (40-60) GeV and a velocity-averaged cross section of O(10^{-26}) cm^{3} s^{-1}. As for the γ-ray data analysis, besides adopting the widely used spatial template fitting, we employ an orthogonal approach with a data-driven spectral template analysis. The fitting to the GeV γ-ray excess yields DM model parameters overlapped with those to fit the antiproton excess via the WW^{*} channel. The consistency of the DM particle properties required to account for the W-boson mass anomaly, the GeV antiproton excess, and the GeV γ-ray excess suggests a common origin of them.
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Affiliation(s)
- Cheng-Rui Zhu
- Key Laboratory of Dark Matter and Space Astronomy, Purple Mountain Observatory, Chinese Academy of Sciences, Nanjing 210023, China
- Shandong Institute of Advanced Technology, Jinan 250100, China
| | - Ming-Yang Cui
- Key Laboratory of Dark Matter and Space Astronomy, Purple Mountain Observatory, Chinese Academy of Sciences, Nanjing 210023, China
| | - Zi-Qing Xia
- Key Laboratory of Dark Matter and Space Astronomy, Purple Mountain Observatory, Chinese Academy of Sciences, Nanjing 210023, China
| | - Zhao-Huan Yu
- School of Physics, Sun Yat-Sen University, Guangzhou 510275, China
| | - Xiaoyuan Huang
- Key Laboratory of Dark Matter and Space Astronomy, Purple Mountain Observatory, Chinese Academy of Sciences, Nanjing 210023, China
- School of Astronomy and Space Science, University of Science and Technology of China, Hefei 230026, Anhui, China
| | - Qiang Yuan
- Key Laboratory of Dark Matter and Space Astronomy, Purple Mountain Observatory, Chinese Academy of Sciences, Nanjing 210023, China
- School of Astronomy and Space Science, University of Science and Technology of China, Hefei 230026, Anhui, China
| | - Yi-Zhong Fan
- Key Laboratory of Dark Matter and Space Astronomy, Purple Mountain Observatory, Chinese Academy of Sciences, Nanjing 210023, China
- School of Astronomy and Space Science, University of Science and Technology of China, Hefei 230026, Anhui, China
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11
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Xu R, Yang L, Yue Q, Kang K, Li Y, Agartioglu M, An H, Chang J, Chen Y, Cheng J, Dai W, Deng Z, Fang C, Geng X, Gong H, Guo X, Guo Q, He L, He S, Hu J, Huang H, Huang T, Jia H, Jiang X, Li H, Li J, Li J, Li Q, Li R, Li X, Li Y, Liang Y, Liao B, Lin F, Lin S, Liu S, Liu Y, Liu Y, Liu Y, Liu Z, Ma H, Mao Y, Nie Q, Ning J, Pan H, Qi N, Ren J, Ruan X, Saraswat K, Sharma V, She Z, Singh M, Sun T, Tang C, Tang W, Tian Y, Wang G, Wang L, Wang Q, Wang Y, Wang Y, Wong H, Wu S, Wu Y, Xing H, Xu Y, Xue T, Yan Y, Yeh C, Yi N, Yu C, Yu H, Yue J, Zeng M, Zeng Z, Zhang B, Zhang F, Zhang L, Zhang Z, Zhang Z, Zhao K, Zhao M, Zhou J, Zhou Z, Zhu J. Constraints on sub-GeV dark matter boosted by cosmic rays from the CDEX-10 experiment at the China Jinping Underground Laboratory. Int J Clin Exp Med 2022. [DOI: 10.1103/physrevd.106.052008] [Citation(s) in RCA: 0] [Impact Index Per Article: 0] [Reference Citation Analysis] [Track Full Text] [Journal Information] [Subscribe] [Scholar Register] [Indexed: 11/07/2022]
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12
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Wang BB, Bi XJ, Fang K, Lin SJ, Yin PF. Solar modulation of cosmic proton and helium with AMS-02. Int J Clin Exp Med 2022. [DOI: 10.1103/physrevd.106.063006] [Citation(s) in RCA: 0] [Impact Index Per Article: 0] [Reference Citation Analysis] [Track Full Text] [Journal Information] [Subscribe] [Scholar Register] [Indexed: 11/07/2022]
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13
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Rankin JS, Bindi V, Bykov AM, Cummings AC, Della Torre S, Florinski V, Heber B, Potgieter MS, Stone EC, Zhang M. Galactic Cosmic Rays Throughout the Heliosphere and in the Very Local Interstellar Medium. SPACE SCIENCE REVIEWS 2022; 218:42. [PMID: 35855211 PMCID: PMC9287243 DOI: 10.1007/s11214-022-00912-4] [Citation(s) in RCA: 0] [Impact Index Per Article: 0] [Reference Citation Analysis] [Abstract] [Grants] [Track Full Text] [Figures] [Subscribe] [Scholar Register] [Received: 03/05/2022] [Accepted: 06/15/2022] [Indexed: 06/15/2023]
Abstract
We review recent observations and modeling developments on the subject of galactic cosmic rays through the heliosphere and in the Very Local Interstellar Medium, emphasizing knowledge that has accumulated over the past decade. We begin by highlighting key measurements of cosmic-ray spectra by Voyager, PAMELA, and AMS and discuss advances in global models of solar modulation. Next, we survey recent works related to large-scale, long-term spatial and temporal variations of cosmic rays in different regimes of the solar wind. Then we highlight new discoveries from beyond the heliopause and link these to the short-term evolution of transients caused by solar activity. Lastly, we visit new results that yield interesting insights from a broader astrophysical perspective.
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Affiliation(s)
- Jamie S. Rankin
- Department of Astrophysical Sciences, Princeton University, Princeton, NJ 08544 USA
| | - Veronica Bindi
- Physics and Astronomy Department, University of Hawaii, Honolulu, HI 96822 USA
| | | | | | | | - Vladimir Florinski
- Center for Space Plasma and Aeronomic Research (CSPAR) and Department of Space Science, University of Alabama in Huntsville, Huntsville, AL 35805 USA
| | - Bernd Heber
- Institute for Experimental and Applied Physics, Christian Albrechts University in Kiel, Kiel, Germany
| | - Marius S. Potgieter
- Institute for Experimental and Applied Physics, Christian Albrechts University in Kiel, Kiel, Germany
| | | | - Ming Zhang
- Department of Physics and Space Sciences, Florida Institute of Technology, Melbourn, FL 32901 USA
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14
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Kleimann J, Dialynas K, Fraternale F, Galli A, Heerikhuisen J, Izmodenov V, Kornbleuth M, Opher M, Pogorelov N. The Structure of the Large-Scale Heliosphere as Seen by Current Models. SPACE SCIENCE REVIEWS 2022; 218:36. [PMID: 35664863 PMCID: PMC9156516 DOI: 10.1007/s11214-022-00902-6] [Citation(s) in RCA: 2] [Impact Index Per Article: 1.0] [Reference Citation Analysis] [Abstract] [Key Words] [Grants] [Track Full Text] [Subscribe] [Scholar Register] [Received: 02/02/2022] [Accepted: 05/06/2022] [Indexed: 05/23/2023]
Abstract
This review summarizes the current state of research aiming at a description of the global heliosphere using both analytical and numerical modeling efforts, particularly in view of the overall plasma/neutral flow and magnetic field structure, and its relation to energetic neutral atoms. Being part of a larger volume on current heliospheric research, it also lays out a number of key concepts and describes several classic, though still relevant early works on the topic. Regarding numerical simulations, emphasis is put on magnetohydrodynamic (MHD), multi-fluid, kinetic-MHD, and hybrid modeling frameworks. Finally, open issues relating to the physical relevance of so-called "croissant" models of the heliosphere, as well as the general (dis)agreement of model predictions with observations are highlighted and critically discussed.
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Affiliation(s)
- Jens Kleimann
- Theoretische Physik IV, Ruhr-Universität Bochum, 44780 Bochum, Germany
| | | | - Federico Fraternale
- Center for Space Plasma and Aeronomic Research, University of Alabama in Huntsville, Huntsville, AL 35899 USA
| | | | - Jacob Heerikhuisen
- Department of Mathematics and Statistics, University of Waikato, Hamilton, 3240 New Zealand
| | - Vladislav Izmodenov
- Moscow Center of Fundamental and Applied Mathematics, Lomonosov Moscow State University, Moscow, Russia
- Space Research Institute (IKI) of Russian Academy of Sciences, Moscow, Russia
| | - Marc Kornbleuth
- Astronomy Department, Boston University, Boston, MA 02215 USA
| | - Merav Opher
- Astronomy Department, Boston University, Boston, MA 02215 USA
- Radcliffe Institute for Advanced Study at Harvard University, Cambridge, MA USA
| | - Nikolai Pogorelov
- Center for Space Plasma and Aeronomic Research, University of Alabama in Huntsville, Huntsville, AL 35899 USA
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15
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Linsky J, Redfield S, Ryder D, Moebius E. Inhomogeneity in the Local ISM and Its Relation to the Heliosphere. SPACE SCIENCE REVIEWS 2022; 218:16. [PMID: 35431347 PMCID: PMC9005448 DOI: 10.1007/s11214-022-00884-5] [Citation(s) in RCA: 1] [Impact Index Per Article: 0.5] [Reference Citation Analysis] [Abstract] [Key Words] [Grants] [Track Full Text] [Subscribe] [Scholar Register] [Received: 01/07/2022] [Accepted: 03/21/2022] [Indexed: 05/23/2023]
Abstract
UNLABELLED This paper reviews past research and new studies underway of the local interstellar environment and its changing influence on the heliosphere. The size, shape, and physical properties of the heliosphere outside of the heliopause are determined by the surrounding environment - now the outer region of the Local Interstellar Cloud (LIC). The temperature, turbulence, and velocity vector of neutral atoms and ions in the LIC and other partially ionized interstellar clouds are measured from high-resolution spectra of interstellar absorption lines observed with the STIS instrument on the HST. Analysis of such spectra led to a kinematic model with many interstellar clouds defined by velocity vectors derived from radial velocity measurements. This analysis identified fifteen clouds located within about 10 pc of the Sun and their mean temperatures, turbulence, and velocity vectors. With the increasing number of sight lines now being analyzed, we find that temperatures and turbulent velocities have spatial variations within the LIC and other nearby clouds much larger than measurement uncertainties, and that these spatial variations appear to be randomly distributed and can be fit by Gaussians. The inhomogeneous length scale is less than 4,000 AU, a distance that the heliosphere will traverse in less than 600 years. The temperatures and turbulent velocities do not show significant trends with stellar distance or angle from the LIC center. If/when the Sun enters an inter-cloud medium, the physical properties of the future heliosphere will be very different from the present. For the heliosheath and the very local interstellar medium (VLISM) just outside of the heliopause, the total pressures are approximately equal to the gravitational pressure of overlying material in the Galaxy. The internal pressure in the LIC is far below that in the VLISM, but there is an uncertain ram pressure term produced by the flow of the LIC with respect to its environment. SUPPLEMENTARY INFORMATION The online version contains supplementary material available at 10.1007/s11214-022-00884-5.
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Affiliation(s)
- Jeffrey Linsky
- JILA, University of Colorado and NIST, Boulder, 80309-0440 CO USA
| | - Seth Redfield
- Astronomy Dept. and Van Vleck Observatory, Wesleyan University, Middletown, 06459-0123 CT USA
| | - Diana Ryder
- Department of Astrophysical and Planetary Sciences, University of Colorado, Boulder, 80309-0391 CO USA
| | - Eberhard Moebius
- Space Science Center and Department of Physics, University of New Hampshire, 8 College Road, Durham, 03824 NH USA
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16
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Adriani O, Akaike Y, Asano K, Asaoka Y, Berti E, Bigongiari G, Binns WR, Bongi M, Brogi P, Bruno A, Buckley JH, Cannady N, Castellini G, Checchia C, Cherry ML, Collazuol G, Ebisawa K, Ficklin AW, Fuke H, Gonzi S, Guzik TG, Hams T, Hibino K, Ichimura M, Ioka K, Ishizaki W, Israel MH, Kasahara K, Kataoka J, Kataoka R, Katayose Y, Kato C, Kawanaka N, Kawakubo Y, Kobayashi K, Kohri K, Krawczynski HS, Krizmanic JF, Maestro P, Marrocchesi PS, Messineo AM, Mitchell JW, Miyake S, Moiseev AA, Mori M, Mori N, Motz HM, Munakata K, Nakahira S, Nishimura J, de Nolfo GA, Okuno S, Ormes JF, Ospina N, Ozawa S, Pacini L, Papini P, Rauch BF, Ricciarini SB, Sakai K, Sakamoto T, Sasaki M, Shimizu Y, Shiomi A, Spillantini P, Stolzi F, Sugita S, Sulaj A, Takita M, Tamura T, Terasawa T, Torii S, Tsunesada Y, Uchihori Y, Vannuccini E, Wefel JP, Yamaoka K, Yanagita S, Yoshida A, Yoshida K, Zober WV. Direct Measurement of the Nickel Spectrum in Cosmic Rays in the Energy Range from 8.8 GeV/n to 240 GeV/n with CALET on the International Space Station. PHYSICAL REVIEW LETTERS 2022; 128:131103. [PMID: 35426700 DOI: 10.1103/physrevlett.128.131103] [Citation(s) in RCA: 1] [Impact Index Per Article: 0.5] [Reference Citation Analysis] [Abstract] [Track Full Text] [Subscribe] [Scholar Register] [Received: 12/27/2021] [Revised: 02/03/2022] [Accepted: 02/28/2022] [Indexed: 06/14/2023]
Abstract
The relative abundance of cosmic ray nickel nuclei with respect to iron is by far larger than for all other transiron elements; therefore it provides a favorable opportunity for a low background measurement of its spectrum. Since nickel, as well as iron, is one of the most stable nuclei, the nickel energy spectrum and its relative abundance with respect to iron provide important information to estimate the abundances at the cosmic ray source and to model the Galactic propagation of heavy nuclei. However, only a few direct measurements of cosmic-ray nickel at energy larger than ∼3 GeV/n are available at present in the literature, and they are affected by strong limitations in both energy reach and statistics. In this Letter, we present a measurement of the differential energy spectrum of nickel in the energy range from 8.8 to 240 GeV/n, carried out with unprecedented precision by the Calorimetric Electron Telescope (CALET) in operation on the International Space Station since 2015. The CALET instrument can identify individual nuclear species via a measurement of their electric charge with a dynamic range extending far beyond iron (up to atomic number Z=40). The particle's energy is measured by a homogeneous calorimeter (1.2 proton interaction lengths, 27 radiation lengths) preceded by a thin imaging section (3 radiation lengths) providing tracking and energy sampling. This Letter follows our previous measurement of the iron spectrum [1O. Adriani et al. (CALET Collaboration), Phys. Rev. Lett. 126, 241101 (2021).PRLTAO0031-900710.1103/PhysRevLett.126.241101], and it extends our investigation on the energy dependence of the spectral index of heavy elements. It reports the analysis of nickel data collected from November 2015 to May 2021 and a detailed assessment of the systematic uncertainties. In the region from 20 to 240 GeV/n our present data are compatible within the errors with a single power law with spectral index -2.51±0.07.
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Affiliation(s)
- O Adriani
- Department of Physics, University of Florence, Via Sansone, 1 - 50019 Sesto Fiorentino, Italy
- INFN Sezione di Florence, Via Sansone, 1 - 50019 Sesto Fiorentino, Italy
| | - Y Akaike
- Waseda Research Institute for Science and Engineering, Waseda University, 17 Kikuicho, Shinjuku, Tokyo 162-0044, Japan
- JEM Utilization Center, Human Spaceflight Technology Directorate, Japan Aerospace Exploration Agency, 2-1-1 Sengen, Tsukuba, Ibaraki 305-8505, Japan
| | - K Asano
- Institute for Cosmic Ray Research, The University of Tokyo, 5-1-5 Kashiwa-no-Ha, Kashiwa, Chiba 277-8582, Japan
| | - Y Asaoka
- Institute for Cosmic Ray Research, The University of Tokyo, 5-1-5 Kashiwa-no-Ha, Kashiwa, Chiba 277-8582, Japan
| | - E Berti
- Department of Physics, University of Florence, Via Sansone, 1 - 50019 Sesto Fiorentino, Italy
- INFN Sezione di Florence, Via Sansone, 1 - 50019 Sesto Fiorentino, Italy
| | - G Bigongiari
- Department of Physical Sciences, Earth and Environment, University of Siena, via Roma 56, 53100 Siena, Italy
- INFN Sezione di Pisa, Polo Fibonacci, Largo B. Pontecorvo, 3 - 56127 Pisa, Italy
| | - W R Binns
- Department of Physics and McDonnell Center for the Space Sciences, Washington University, One Brookings Drive, St. Louis, Missouri 63130-4899, USA
| | - M Bongi
- Department of Physics, University of Florence, Via Sansone, 1 - 50019 Sesto Fiorentino, Italy
- INFN Sezione di Florence, Via Sansone, 1 - 50019 Sesto Fiorentino, Italy
| | - P Brogi
- Department of Physical Sciences, Earth and Environment, University of Siena, via Roma 56, 53100 Siena, Italy
- INFN Sezione di Pisa, Polo Fibonacci, Largo B. Pontecorvo, 3 - 56127 Pisa, Italy
| | - A Bruno
- Heliospheric Physics Laboratory, NASA/GSFC, Greenbelt, Maryland 20771, USA
| | - J H Buckley
- Department of Physics and McDonnell Center for the Space Sciences, Washington University, One Brookings Drive, St. Louis, Missouri 63130-4899, USA
| | - N Cannady
- Center for Space Sciences and Technology, University of Maryland, Baltimore County, 1000 Hilltop Circle, Baltimore, Maryland 21250, USA
- Astroparticle Physics Laboratory, NASA/GSFC, Greenbelt, Maryland 20771, USA
- Center for Research and Exploration in Space Sciences and Technology, NASA/GSFC, Greenbelt, Maryland 20771, USA
| | - G Castellini
- Institute of Applied Physics (IFAC), National Research Council (CNR), Via Madonna del Piano, 10, 50019 Sesto Fiorentino, Italy
| | - C Checchia
- Department of Physical Sciences, Earth and Environment, University of Siena, via Roma 56, 53100 Siena, Italy
- INFN Sezione di Pisa, Polo Fibonacci, Largo B. Pontecorvo, 3 - 56127 Pisa, Italy
| | - M L Cherry
- Department of Physics and Astronomy, Louisiana State University, 202 Nicholson Hall, Baton Rouge, Louisiana 70803, USA
| | - G Collazuol
- Department of Physics and Astronomy, University of Padova, Via Marzolo, 8, 35131 Padova, Italy
- INFN Sezione di Padova, Via Marzolo, 8, 35131 Padova, Italy
| | - K Ebisawa
- Institute of Space and Astronautical Science, Japan Aerospace Exploration Agency, 3-1-1 Yoshinodai, Chuo, Sagamihara, Kanagawa 252-5210, Japan
| | - A W Ficklin
- Department of Physics and Astronomy, Louisiana State University, 202 Nicholson Hall, Baton Rouge, Louisiana 70803, USA
| | - H Fuke
- Institute of Space and Astronautical Science, Japan Aerospace Exploration Agency, 3-1-1 Yoshinodai, Chuo, Sagamihara, Kanagawa 252-5210, Japan
| | - S Gonzi
- Department of Physics, University of Florence, Via Sansone, 1 - 50019 Sesto Fiorentino, Italy
- INFN Sezione di Florence, Via Sansone, 1 - 50019 Sesto Fiorentino, Italy
| | - T G Guzik
- Department of Physics and Astronomy, Louisiana State University, 202 Nicholson Hall, Baton Rouge, Louisiana 70803, USA
| | - T Hams
- Center for Space Sciences and Technology, University of Maryland, Baltimore County, 1000 Hilltop Circle, Baltimore, Maryland 21250, USA
| | - K Hibino
- Kanagawa University, 3-27-1 Rokkakubashi, Kanagawa, Yokohama, Kanagawa 221-8686, Japan
| | - M Ichimura
- Faculty of Science and Technology, Graduate School of Science and Technology, Hirosaki University, 3, Bunkyo, Hirosaki, Aomori 036-8561, Japan
| | - K Ioka
- Yukawa Institute for Theoretical Physics, Kyoto University, Kitashirakawa Oiwake-cho, Sakyo-ku, Kyoto 606-8502, Japan
| | - W Ishizaki
- Institute for Cosmic Ray Research, The University of Tokyo, 5-1-5 Kashiwa-no-Ha, Kashiwa, Chiba 277-8582, Japan
| | - M H Israel
- Department of Physics and McDonnell Center for the Space Sciences, Washington University, One Brookings Drive, St. Louis, Missouri 63130-4899, USA
| | - K Kasahara
- Department of Electronic Information Systems, Shibaura Institute of Technology, 307 Fukasaku, Minuma, Saitama 337-8570, Japan
| | - J Kataoka
- School of Advanced Science and Engineering, Waseda University, 3-4-1 Okubo, Shinjuku, Tokyo 169-8555, Japan
| | - R Kataoka
- National Institute of Polar Research, 10-3, Midori-cho, Tachikawa, Tokyo 190-8518, Japan
| | - Y Katayose
- Faculty of Engineering, Division of Intelligent Systems Engineering, Yokohama National University, 79-5 Tokiwadai, Hodogaya, Yokohama 240-8501, Japan
| | - C Kato
- Faculty of Science, Shinshu University, 3-1-1 Asahi, Matsumoto, Nagano 390-8621, Japan
| | - N Kawanaka
- Yukawa Institute for Theoretical Physics, Kyoto University, Kitashirakawa Oiwake-cho, Sakyo-ku, Kyoto 606-8502, Japan
- Department of Astronomy, Graduate School of Science, Kyoto University, Kitashirakawa Oiwake-cho, Sakyo-ku, Kyoto 606-8502, Japan
| | - Y Kawakubo
- Department of Physics and Astronomy, Louisiana State University, 202 Nicholson Hall, Baton Rouge, Louisiana 70803, USA
| | - K Kobayashi
- Waseda Research Institute for Science and Engineering, Waseda University, 17 Kikuicho, Shinjuku, Tokyo 162-0044, Japan
- JEM Utilization Center, Human Spaceflight Technology Directorate, Japan Aerospace Exploration Agency, 2-1-1 Sengen, Tsukuba, Ibaraki 305-8505, Japan
| | - K Kohri
- Institute of Particle and Nuclear Studies, High Energy Accelerator Research Organization, 1-1 Oho, Tsukuba, Ibaraki 305-0801, Japan
| | - H S Krawczynski
- Department of Physics and McDonnell Center for the Space Sciences, Washington University, One Brookings Drive, St. Louis, Missouri 63130-4899, USA
| | - J F Krizmanic
- Astroparticle Physics Laboratory, NASA/GSFC, Greenbelt, Maryland 20771, USA
| | - P Maestro
- Department of Physical Sciences, Earth and Environment, University of Siena, via Roma 56, 53100 Siena, Italy
- INFN Sezione di Pisa, Polo Fibonacci, Largo B. Pontecorvo, 3 - 56127 Pisa, Italy
| | - P S Marrocchesi
- Department of Physical Sciences, Earth and Environment, University of Siena, via Roma 56, 53100 Siena, Italy
- INFN Sezione di Pisa, Polo Fibonacci, Largo B. Pontecorvo, 3 - 56127 Pisa, Italy
| | - A M Messineo
- INFN Sezione di Pisa, Polo Fibonacci, Largo B. Pontecorvo, 3 - 56127 Pisa, Italy
- University of Pisa, Polo Fibonacci, Largo B. Pontecorvo, 3 - 56127 Pisa, Italy
| | - J W Mitchell
- Astroparticle Physics Laboratory, NASA/GSFC, Greenbelt, Maryland 20771, USA
| | - S Miyake
- Department of Electrical and Electronic Systems Engineering, National Institute of Technology, Ibaraki College, 866 Nakane, Hitachinaka, Ibaraki 312-8508, Japan
| | - A A Moiseev
- Astroparticle Physics Laboratory, NASA/GSFC, Greenbelt, Maryland 20771, USA
- Center for Research and Exploration in Space Sciences and Technology, NASA/GSFC, Greenbelt, Maryland 20771, USA
- Department of Astronomy, University of Maryland, College Park, Maryland 20742, USA
| | - M Mori
- Department of Physical Sciences, College of Science and Engineering, Ritsumeikan University, Shiga 525-8577, Japan
| | - N Mori
- INFN Sezione di Florence, Via Sansone, 1 - 50019 Sesto Fiorentino, Italy
| | - H M Motz
- Faculty of Science and Engineering, Global Center for Science and Engineering, Waseda University, 3-4-1 Okubo, Shinjuku, Tokyo 169-8555, Japan
| | - K Munakata
- Faculty of Science, Shinshu University, 3-1-1 Asahi, Matsumoto, Nagano 390-8621, Japan
| | - S Nakahira
- Institute of Space and Astronautical Science, Japan Aerospace Exploration Agency, 3-1-1 Yoshinodai, Chuo, Sagamihara, Kanagawa 252-5210, Japan
| | - J Nishimura
- Institute of Space and Astronautical Science, Japan Aerospace Exploration Agency, 3-1-1 Yoshinodai, Chuo, Sagamihara, Kanagawa 252-5210, Japan
| | - G A de Nolfo
- Heliospheric Physics Laboratory, NASA/GSFC, Greenbelt, Maryland 20771, USA
| | - S Okuno
- Kanagawa University, 3-27-1 Rokkakubashi, Kanagawa, Yokohama, Kanagawa 221-8686, Japan
| | - J F Ormes
- Department of Physics and Astronomy, University of Denver, Physics Building, Room 211, 2112 East Wesley Avenue, Denver, Colorado 80208-6900, USA
| | - N Ospina
- Department of Physics and Astronomy, University of Padova, Via Marzolo, 8, 35131 Padova, Italy
- INFN Sezione di Padova, Via Marzolo, 8, 35131 Padova, Italy
| | - S Ozawa
- Quantum ICT Advanced Development Center, National Institute of Information and Communications Technology, 4-2-1 Nukui-Kitamachi, Koganei, Tokyo 184-8795, Japan
| | - L Pacini
- Department of Physics, University of Florence, Via Sansone, 1 - 50019 Sesto Fiorentino, Italy
- INFN Sezione di Florence, Via Sansone, 1 - 50019 Sesto Fiorentino, Italy
- Institute of Applied Physics (IFAC), National Research Council (CNR), Via Madonna del Piano, 10, 50019 Sesto Fiorentino, Italy
| | - P Papini
- INFN Sezione di Florence, Via Sansone, 1 - 50019 Sesto Fiorentino, Italy
| | - B F Rauch
- Department of Physics and McDonnell Center for the Space Sciences, Washington University, One Brookings Drive, St. Louis, Missouri 63130-4899, USA
| | - S B Ricciarini
- INFN Sezione di Florence, Via Sansone, 1 - 50019 Sesto Fiorentino, Italy
- Institute of Applied Physics (IFAC), National Research Council (CNR), Via Madonna del Piano, 10, 50019 Sesto Fiorentino, Italy
| | - K Sakai
- Center for Space Sciences and Technology, University of Maryland, Baltimore County, 1000 Hilltop Circle, Baltimore, Maryland 21250, USA
- Astroparticle Physics Laboratory, NASA/GSFC, Greenbelt, Maryland 20771, USA
- Center for Research and Exploration in Space Sciences and Technology, NASA/GSFC, Greenbelt, Maryland 20771, USA
| | - T Sakamoto
- College of Science and Engineering, Department of Physics and Mathematics, Aoyama Gakuin University, 5-10-1 Fuchinobe, Chuo, Sagamihara, Kanagawa 252-5258, Japan
| | - M Sasaki
- Astroparticle Physics Laboratory, NASA/GSFC, Greenbelt, Maryland 20771, USA
- Center for Research and Exploration in Space Sciences and Technology, NASA/GSFC, Greenbelt, Maryland 20771, USA
- Department of Astronomy, University of Maryland, College Park, Maryland 20742, USA
| | - Y Shimizu
- Kanagawa University, 3-27-1 Rokkakubashi, Kanagawa, Yokohama, Kanagawa 221-8686, Japan
| | - A Shiomi
- College of Industrial Technology, Nihon University, 1-2-1 Izumi, Narashino, Chiba 275-8575, Japan
| | - P Spillantini
- Department of Physics, University of Florence, Via Sansone, 1 - 50019 Sesto Fiorentino, Italy
| | - F Stolzi
- Department of Physical Sciences, Earth and Environment, University of Siena, via Roma 56, 53100 Siena, Italy
- INFN Sezione di Pisa, Polo Fibonacci, Largo B. Pontecorvo, 3 - 56127 Pisa, Italy
| | - S Sugita
- College of Science and Engineering, Department of Physics and Mathematics, Aoyama Gakuin University, 5-10-1 Fuchinobe, Chuo, Sagamihara, Kanagawa 252-5258, Japan
| | - A Sulaj
- Department of Physical Sciences, Earth and Environment, University of Siena, via Roma 56, 53100 Siena, Italy
- INFN Sezione di Pisa, Polo Fibonacci, Largo B. Pontecorvo, 3 - 56127 Pisa, Italy
| | - M Takita
- Institute for Cosmic Ray Research, The University of Tokyo, 5-1-5 Kashiwa-no-Ha, Kashiwa, Chiba 277-8582, Japan
| | - T Tamura
- Kanagawa University, 3-27-1 Rokkakubashi, Kanagawa, Yokohama, Kanagawa 221-8686, Japan
| | - T Terasawa
- Institute for Cosmic Ray Research, The University of Tokyo, 5-1-5 Kashiwa-no-Ha, Kashiwa, Chiba 277-8582, Japan
| | - S Torii
- Waseda Research Institute for Science and Engineering, Waseda University, 17 Kikuicho, Shinjuku, Tokyo 162-0044, Japan
| | - Y Tsunesada
- Division of Mathematics and Physics, Graduate School of Science, Osaka City University, 3-3-138 Sugimoto, Sumiyoshi, Osaka 558-8585, Japan
- Nambu Yoichiro Institute of Theoretical and Experimental Physics, Osaka City University, 3-3-138 Sugimoto, Sumiyoshi, Osaka 558-8585, Japan
| | - Y Uchihori
- National Institutes for Quantum and Radiation Science and Technology, 4-9-1 Anagawa, Inage, Chiba 263-8555, Japan
| | - E Vannuccini
- INFN Sezione di Florence, Via Sansone, 1 - 50019 Sesto Fiorentino, Italy
| | - J P Wefel
- Department of Physics and Astronomy, Louisiana State University, 202 Nicholson Hall, Baton Rouge, Louisiana 70803, USA
| | - K Yamaoka
- Nagoya University, Furo, Chikusa, Nagoya 464-8601, Japan
| | - S Yanagita
- College of Science, Ibaraki University, 2-1-1 Bunkyo, Mito, Ibaraki 310-8512, Japan
| | - A Yoshida
- College of Science and Engineering, Department of Physics and Mathematics, Aoyama Gakuin University, 5-10-1 Fuchinobe, Chuo, Sagamihara, Kanagawa 252-5258, Japan
| | - K Yoshida
- Department of Electronic Information Systems, Shibaura Institute of Technology, 307 Fukasaku, Minuma, Saitama 337-8570, Japan
| | - W V Zober
- Department of Physics and McDonnell Center for the Space Sciences, Washington University, One Brookings Drive, St. Louis, Missouri 63130-4899, USA
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17
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Aharonian F, Ait Benkhali F, Angüner EO, Ashkar H, Backes M, Baghmanyan V, Barbosa Martins V, Batzofin R, Becherini Y, Berge D, Bernlöhr K, Bi B, Böttcher M, Boisson C, Bolmont J, de Bony de Lavergne M, Breuhaus M, Brose R, Brun F, Caroff S, Casanova S, Cerruti M, Chand T, Chen A, Cotter G, Damascene Mbarubucyeye J, Djannati-Ataï A, Dmytriiev A, Doroshenko V, Duffy C, Egberts K, Ernenwein JP, Fegan S, Feijen K, Fiasson A, Fichet de Clairfontaine G, Fontaine G, Füßling M, Funk S, Gabici S, Gallant YA, Ghafourizadeh S, Giavitto G, Giunti L, Glawion D, Glicenstein JF, Grondin MH, Hermann G, Hinton JA, Hörbe M, Hofmann W, Hoischen C, Holch TL, Holler M, Horns D, Huang Z, Jamrozy M, Jankowsky F, Jung-Richardt I, Kasai E, Katarzyński K, Katz U, Khangulyan D, Khélifi B, Klepser S, Kluźniak W, Komin N, Konno R, Kosack K, Kostunin D, Le Stum S, Lemière A, Lemoine-Goumard M, Lenain JP, Leuschner F, Lohse T, Luashvili A, Lypova I, Mackey J, Malyshev D, Malyshev D, Marandon V, Marchegiani P, Marcowith A, Martí-Devesa G, Marx R, Maurin G, Meyer M, Mitchell A, Moderski R, Mohrmann L, Montanari A, Moulin E, Muller J, Murach T, Nakashima K, de Naurois M, Nayerhoda A, Niemiec J, Priyana Noel A, O'Brien P, Ohm S, Olivera-Nieto L, de Ona Wilhelmi E, Ostrowski M, Panny S, Panter M, Parsons RD, Peron G, Pita S, Poireau V, Prokhorov DA, Prokoph H, Pühlhofer G, Punch M, Quirrenbach A, Reichherzer P, Reimer A, Reimer O, Renaud M, Reville B, Rieger F, Rowell G, Rudak B, Rueda Ricarte H, Ruiz-Velasco E, Sahakian V, Sailer S, Salzmann H, Sanchez DA, Santangelo A, Sasaki M, Schäfer J, Schüssler F, Schutte HM, Schwanke U, Senniappan M, Shapopi JNS, Simoni R, Sinha A, Sol H, Specovius A, Spencer S, Stawarz Ł, Steinmassl S, Steppa C, Takahashi T, Tanaka T, Taylor AM, Terrier R, Thorpe-Morgan C, Tsirou M, Tsuji N, Tuffs R, Uchiyama Y, Unbehaun T, van Eldik C, van Soelen B, Veh J, Venter C, Vink J, Wagner SJ, Werner F, White R, Wierzcholska A, Wong YW, Yusafzai A, Zacharias M, Zargaryan D, Zdziarski AA, Zech A, Zhu SJ, Zouari S, Żywucka N. Time-resolved hadronic particle acceleration in the recurrent nova RS Ophiuchi. Science 2022; 376:77-80. [PMID: 35271303 DOI: 10.1126/science.abn0567] [Citation(s) in RCA: 11] [Impact Index Per Article: 5.5] [Reference Citation Analysis] [Abstract] [Track Full Text] [Journal Information] [Subscribe] [Scholar Register] [Indexed: 11/02/2022]
Abstract
Recurrent novae are repeating thermonuclear explosions in the outer layers of white dwarfs, due to the accretion of fresh material from a binary companion. The shock generated when ejected material slams into the companion star's wind can accelerate particles. We report very-high-energy (VHE, [Formula: see text]) gamma rays from the recurrent nova RS Ophiuchi, up to a month after its 2021 outburst, observed using the High Energy Stereoscopic System. The VHE emission has a similar temporal profile to lower-energy GeV emission, indicating a common origin, with a two-day delay in peak flux. These observations constrain models of time-dependent particle energization, favoring a hadronic emission scenario over the leptonic alternative. Shocks in dense winds provide favorable environments for efficient acceleration of cosmic-rays to very high energies.
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Affiliation(s)
- F Aharonian
- Dublin Institute for Advanced Studies, 31 Fitzwilliam Place, Dublin 2, Ireland
- Max-Planck-Institut für Kernphysik, P.O. Box 103980, D 69029 Heidelberg, Germany
- High Energy Astrophysics Laboratory, Russian-Armenian University (RAU), 123 Hovsep Emin St Yerevan 0051, Armenia
| | - F Ait Benkhali
- Landessternwarte, Universität Heidelberg, Königstuhl, D 69117 Heidelberg, Germany
| | - E O Angüner
- Aix Marseille Université, Centre national de la recherche scientifique (CNRS)/Institut National de Physique Nucléaire et Physique des Particules (IN2P3), Centre de Physique des Particules de Marseille (CPPM), Marseille, France
| | - H Ashkar
- Laboratoire Leprince-Ringuet, École Polytechnique, CNRS, Institut Polytechnique de Paris, F-91128 Palaiseau, France
| | - M Backes
- University of Namibia, Department of Physics, Private Bag 13301, Windhoek 10005, Namibia
- Centre for Space Research, North-West University, Potchefstroom 2520, South Africa
| | - V Baghmanyan
- Instytut Fizyki J[Formula: see text]drowej Polskiej Akademii Nauk (PAN), ul. Radzikowskiego 152, 31-342 Kraków, Poland
| | - V Barbosa Martins
- Deutsches Elektronen-Synchrotron DESY, Platanenallee 6, 15738, Germany
| | - R Batzofin
- School of Physics, University of the Witwatersrand, 1 Jan Smuts Avenue, Braamfontein, Johannesburg, 2050 South Africa
| | - Y Becherini
- Université de Paris, CNRS, Astroparticule et Cosmologie, F-75013 Paris, France
- Department of Physics and Electrical Engineering, Linnaeus University, 351 95 Växjö, Sweden
| | - D Berge
- Deutsches Elektronen-Synchrotron DESY, Platanenallee 6, 15738, Germany
| | - K Bernlöhr
- Max-Planck-Institut für Kernphysik, P.O. Box 103980, D 69029 Heidelberg, Germany
| | - B Bi
- Institut für Astronomie und Astrophysik, Universität Tübingen, Sand 1, D 72076 Tübingen, Germany
| | - M Böttcher
- Centre for Space Research, North-West University, Potchefstroom 2520, South Africa
| | - C Boisson
- Laboratoire Univers et Théories, Observatoire de Paris, Université PSL, CNRS, Université de Paris, 92190 Meudon, France
| | - J Bolmont
- Sorbonne Université, Université Paris Diderot, Sorbonne Paris Cité, CNRS/IN2P3, Laboratoire de Physique Nucléaire et de Hautes Energies (LPNHE), 4 Place Jussieu, F-75252 Paris, France
| | - M de Bony de Lavergne
- Université Savoie Mont Blanc, CNRS, Laboratoire d'Annecy de Physique des Particules - IN2P3, 74000 Annecy, France
| | - M Breuhaus
- Max-Planck-Institut für Kernphysik, P.O. Box 103980, D 69029 Heidelberg, Germany
| | - R Brose
- Dublin Institute for Advanced Studies, 31 Fitzwilliam Place, Dublin 2, Ireland
| | - F Brun
- Institute for Research on the Fundamental Laws of the Universe (IRFU), Commisariat à l'énergie atomique (CEA), Université Paris-Saclay, F-91191 Gif-sur-Yvette, France
| | - S Caroff
- Sorbonne Université, Université Paris Diderot, Sorbonne Paris Cité, CNRS/IN2P3, Laboratoire de Physique Nucléaire et de Hautes Energies (LPNHE), 4 Place Jussieu, F-75252 Paris, France
| | - S Casanova
- Instytut Fizyki J[Formula: see text]drowej Polskiej Akademii Nauk (PAN), ul. Radzikowskiego 152, 31-342 Kraków, Poland
| | - M Cerruti
- Université de Paris, CNRS, Astroparticule et Cosmologie, F-75013 Paris, France
| | - T Chand
- Centre for Space Research, North-West University, Potchefstroom 2520, South Africa
| | - A Chen
- School of Physics, University of the Witwatersrand, 1 Jan Smuts Avenue, Braamfontein, Johannesburg, 2050 South Africa
| | - G Cotter
- University of Oxford, Department of Physics, Denys Wilkinson Building, Keble Road, Oxford OX1 3RH, UK
| | | | - A Djannati-Ataï
- Université de Paris, CNRS, Astroparticule et Cosmologie, F-75013 Paris, France
| | - A Dmytriiev
- Laboratoire Univers et Théories, Observatoire de Paris, Université PSL, CNRS, Université de Paris, 92190 Meudon, France
| | - V Doroshenko
- Institut für Astronomie und Astrophysik, Universität Tübingen, Sand 1, D 72076 Tübingen, Germany
| | - C Duffy
- University of Oxford, Department of Physics, Denys Wilkinson Building, Keble Road, Oxford OX1 3RH, UK
| | - K Egberts
- Institut für Physik und Astronomie, Universität Potsdam, Karl-Liebknecht-Strasse 24/25, D 14476 Potsdam, Germany
| | - J-P Ernenwein
- Aix Marseille Université, Centre national de la recherche scientifique (CNRS)/Institut National de Physique Nucléaire et Physique des Particules (IN2P3), Centre de Physique des Particules de Marseille (CPPM), Marseille, France
| | - S Fegan
- Laboratoire Leprince-Ringuet, École Polytechnique, CNRS, Institut Polytechnique de Paris, F-91128 Palaiseau, France
| | - K Feijen
- School of Physical Sciences, University of Adelaide, Adelaide 5005, Australia
| | - A Fiasson
- Université Savoie Mont Blanc, CNRS, Laboratoire d'Annecy de Physique des Particules - IN2P3, 74000 Annecy, France
| | - G Fichet de Clairfontaine
- Laboratoire Univers et Théories, Observatoire de Paris, Université PSL, CNRS, Université de Paris, 92190 Meudon, France
| | - G Fontaine
- Laboratoire Leprince-Ringuet, École Polytechnique, CNRS, Institut Polytechnique de Paris, F-91128 Palaiseau, France
| | - M Füßling
- Deutsches Elektronen-Synchrotron DESY, Platanenallee 6, 15738, Germany
| | - S Funk
- Friedrich-Alexander-Universität Erlangen-Nürnberg, Erlangen Centre for Astroparticle Physics, Erwin-Rommel-Str. 1, D 91058 Erlangen, Germany
| | - S Gabici
- Université de Paris, CNRS, Astroparticule et Cosmologie, F-75013 Paris, France
| | - Y A Gallant
- Laboratoire Univers et Particules de Montpellier, Université Montpellier, CNRS/IN2P3, CC 72, Place Eugène Bataillon, F-34095 Montpellier Cedex 5, France
| | - S Ghafourizadeh
- Landessternwarte, Universität Heidelberg, Königstuhl, D 69117 Heidelberg, Germany
| | - G Giavitto
- Deutsches Elektronen-Synchrotron DESY, Platanenallee 6, 15738, Germany
| | - L Giunti
- Université de Paris, CNRS, Astroparticule et Cosmologie, F-75013 Paris, France
- Institute for Research on the Fundamental Laws of the Universe (IRFU), Commisariat à l'énergie atomique (CEA), Université Paris-Saclay, F-91191 Gif-sur-Yvette, France
| | - D Glawion
- Friedrich-Alexander-Universität Erlangen-Nürnberg, Erlangen Centre for Astroparticle Physics, Erwin-Rommel-Str. 1, D 91058 Erlangen, Germany
| | - J F Glicenstein
- Institute for Research on the Fundamental Laws of the Universe (IRFU), Commisariat à l'énergie atomique (CEA), Université Paris-Saclay, F-91191 Gif-sur-Yvette, France
| | - M-H Grondin
- Université Bordeaux, CNRS, Laboratoire de Physique des Deux Infinis (LP2i), Bordeaux, Joint Research Unit (UMR 5797), F-33170 Gradignan, France
| | - G Hermann
- Max-Planck-Institut für Kernphysik, P.O. Box 103980, D 69029 Heidelberg, Germany
| | - J A Hinton
- Max-Planck-Institut für Kernphysik, P.O. Box 103980, D 69029 Heidelberg, Germany
| | - M Hörbe
- University of Oxford, Department of Physics, Denys Wilkinson Building, Keble Road, Oxford OX1 3RH, UK
| | - W Hofmann
- Max-Planck-Institut für Kernphysik, P.O. Box 103980, D 69029 Heidelberg, Germany
| | - C Hoischen
- Institut für Physik und Astronomie, Universität Potsdam, Karl-Liebknecht-Strasse 24/25, D 14476 Potsdam, Germany
| | - T L Holch
- Deutsches Elektronen-Synchrotron DESY, Platanenallee 6, 15738, Germany
| | - M Holler
- Institut für Astro- und Teilchenphysik, Leopold-Franzens-Universität Innsbruck, A-6020 Innsbruck, Austria
| | - D Horns
- Universität Hamburg, Institut für Experimentalphysik, Luruper Chaussee 149, D 22761 Hamburg, Germany
| | - Zhiqiu Huang
- Max-Planck-Institut für Kernphysik, P.O. Box 103980, D 69029 Heidelberg, Germany
| | - M Jamrozy
- Obserwatorium Astronomiczne, Uniwersytet Jagielloński, ul. Orla 171, 30-244 Kraków, Poland
| | - F Jankowsky
- Landessternwarte, Universität Heidelberg, Königstuhl, D 69117 Heidelberg, Germany
| | - I Jung-Richardt
- Friedrich-Alexander-Universität Erlangen-Nürnberg, Erlangen Centre for Astroparticle Physics, Erwin-Rommel-Str. 1, D 91058 Erlangen, Germany
| | - E Kasai
- University of Namibia, Department of Physics, Private Bag 13301, Windhoek 10005, Namibia
| | - K Katarzyński
- Institute of Astronomy, Faculty of Physics, Astronomy and Informatics, Nicolaus Copernicus University, Grudziadzka 5, 87-100 Torun, Poland
| | - U Katz
- Friedrich-Alexander-Universität Erlangen-Nürnberg, Erlangen Centre for Astroparticle Physics, Erwin-Rommel-Str. 1, D 91058 Erlangen, Germany
| | - D Khangulyan
- Department of Physics, Rikkyo University, 3-34-1 Nishi-Ikebukuro, Toshima-ku, Tokyo 171-8501, Japan
| | - B Khélifi
- Université de Paris, CNRS, Astroparticule et Cosmologie, F-75013 Paris, France
| | - S Klepser
- Deutsches Elektronen-Synchrotron DESY, Platanenallee 6, 15738, Germany
| | - W Kluźniak
- Nicolaus Copernicus Astronomical Center, Polish Academy of Sciences, ul. Bartycka 18, 00-716 Warsaw, Poland
| | - Nu Komin
- School of Physics, University of the Witwatersrand, 1 Jan Smuts Avenue, Braamfontein, Johannesburg, 2050 South Africa
| | - R Konno
- Deutsches Elektronen-Synchrotron DESY, Platanenallee 6, 15738, Germany
| | - K Kosack
- Institute for Research on the Fundamental Laws of the Universe (IRFU), Commisariat à l'énergie atomique (CEA), Université Paris-Saclay, F-91191 Gif-sur-Yvette, France
| | - D Kostunin
- Deutsches Elektronen-Synchrotron DESY, Platanenallee 6, 15738, Germany
| | - S Le Stum
- Aix Marseille Université, Centre national de la recherche scientifique (CNRS)/Institut National de Physique Nucléaire et Physique des Particules (IN2P3), Centre de Physique des Particules de Marseille (CPPM), Marseille, France
| | - A Lemière
- Université de Paris, CNRS, Astroparticule et Cosmologie, F-75013 Paris, France
| | - M Lemoine-Goumard
- Université Bordeaux, CNRS, Laboratoire de Physique des Deux Infinis (LP2i), Bordeaux, Joint Research Unit (UMR 5797), F-33170 Gradignan, France
| | - J-P Lenain
- Sorbonne Université, Université Paris Diderot, Sorbonne Paris Cité, CNRS/IN2P3, Laboratoire de Physique Nucléaire et de Hautes Energies (LPNHE), 4 Place Jussieu, F-75252 Paris, France
| | - F Leuschner
- Institut für Astronomie und Astrophysik, Universität Tübingen, Sand 1, D 72076 Tübingen, Germany
| | - T Lohse
- Institut für Physik, Humboldt-Universität zu Berlin, Newtonstr. 15, D 12489 Berlin, Germany
| | - A Luashvili
- Laboratoire Univers et Théories, Observatoire de Paris, Université PSL, CNRS, Université de Paris, 92190 Meudon, France
| | - I Lypova
- Landessternwarte, Universität Heidelberg, Königstuhl, D 69117 Heidelberg, Germany
| | - J Mackey
- Dublin Institute for Advanced Studies, 31 Fitzwilliam Place, Dublin 2, Ireland
| | - D Malyshev
- Institut für Astronomie und Astrophysik, Universität Tübingen, Sand 1, D 72076 Tübingen, Germany
| | - D Malyshev
- Friedrich-Alexander-Universität Erlangen-Nürnberg, Erlangen Centre for Astroparticle Physics, Erwin-Rommel-Str. 1, D 91058 Erlangen, Germany
| | - V Marandon
- Max-Planck-Institut für Kernphysik, P.O. Box 103980, D 69029 Heidelberg, Germany
| | - P Marchegiani
- School of Physics, University of the Witwatersrand, 1 Jan Smuts Avenue, Braamfontein, Johannesburg, 2050 South Africa
| | - A Marcowith
- Laboratoire Univers et Particules de Montpellier, Université Montpellier, CNRS/IN2P3, CC 72, Place Eugène Bataillon, F-34095 Montpellier Cedex 5, France
| | - G Martí-Devesa
- Institut für Astro- und Teilchenphysik, Leopold-Franzens-Universität Innsbruck, A-6020 Innsbruck, Austria
| | - R Marx
- Landessternwarte, Universität Heidelberg, Königstuhl, D 69117 Heidelberg, Germany
| | - G Maurin
- Université Savoie Mont Blanc, CNRS, Laboratoire d'Annecy de Physique des Particules - IN2P3, 74000 Annecy, France
| | - M Meyer
- Universität Hamburg, Institut für Experimentalphysik, Luruper Chaussee 149, D 22761 Hamburg, Germany
| | - A Mitchell
- Max-Planck-Institut für Kernphysik, P.O. Box 103980, D 69029 Heidelberg, Germany
- Friedrich-Alexander-Universität Erlangen-Nürnberg, Erlangen Centre for Astroparticle Physics, Erwin-Rommel-Str. 1, D 91058 Erlangen, Germany
| | - R Moderski
- Nicolaus Copernicus Astronomical Center, Polish Academy of Sciences, ul. Bartycka 18, 00-716 Warsaw, Poland
| | - L Mohrmann
- Max-Planck-Institut für Kernphysik, P.O. Box 103980, D 69029 Heidelberg, Germany
| | - A Montanari
- Institute for Research on the Fundamental Laws of the Universe (IRFU), Commisariat à l'énergie atomique (CEA), Université Paris-Saclay, F-91191 Gif-sur-Yvette, France
| | - E Moulin
- Institute for Research on the Fundamental Laws of the Universe (IRFU), Commisariat à l'énergie atomique (CEA), Université Paris-Saclay, F-91191 Gif-sur-Yvette, France
| | - J Muller
- Laboratoire Leprince-Ringuet, École Polytechnique, CNRS, Institut Polytechnique de Paris, F-91128 Palaiseau, France
| | - T Murach
- Deutsches Elektronen-Synchrotron DESY, Platanenallee 6, 15738, Germany
| | - K Nakashima
- Friedrich-Alexander-Universität Erlangen-Nürnberg, Erlangen Centre for Astroparticle Physics, Erwin-Rommel-Str. 1, D 91058 Erlangen, Germany
| | - M de Naurois
- Laboratoire Leprince-Ringuet, École Polytechnique, CNRS, Institut Polytechnique de Paris, F-91128 Palaiseau, France
| | - A Nayerhoda
- Instytut Fizyki J[Formula: see text]drowej Polskiej Akademii Nauk (PAN), ul. Radzikowskiego 152, 31-342 Kraków, Poland
| | - J Niemiec
- Instytut Fizyki J[Formula: see text]drowej Polskiej Akademii Nauk (PAN), ul. Radzikowskiego 152, 31-342 Kraków, Poland
| | - A Priyana Noel
- Obserwatorium Astronomiczne, Uniwersytet Jagielloński, ul. Orla 171, 30-244 Kraków, Poland
| | - P O'Brien
- Department of Physics and Astronomy, The University of Leicester, University Road, Leicester, LE1 7RH, UK
| | - S Ohm
- Deutsches Elektronen-Synchrotron DESY, Platanenallee 6, 15738, Germany
| | - L Olivera-Nieto
- Max-Planck-Institut für Kernphysik, P.O. Box 103980, D 69029 Heidelberg, Germany
| | - E de Ona Wilhelmi
- Deutsches Elektronen-Synchrotron DESY, Platanenallee 6, 15738, Germany
| | - M Ostrowski
- Obserwatorium Astronomiczne, Uniwersytet Jagielloński, ul. Orla 171, 30-244 Kraków, Poland
| | - S Panny
- Institut für Astro- und Teilchenphysik, Leopold-Franzens-Universität Innsbruck, A-6020 Innsbruck, Austria
| | - M Panter
- Max-Planck-Institut für Kernphysik, P.O. Box 103980, D 69029 Heidelberg, Germany
| | - R D Parsons
- Institut für Physik, Humboldt-Universität zu Berlin, Newtonstr. 15, D 12489 Berlin, Germany
| | - G Peron
- Max-Planck-Institut für Kernphysik, P.O. Box 103980, D 69029 Heidelberg, Germany
| | - S Pita
- Université de Paris, CNRS, Astroparticule et Cosmologie, F-75013 Paris, France
| | - V Poireau
- Université Savoie Mont Blanc, CNRS, Laboratoire d'Annecy de Physique des Particules - IN2P3, 74000 Annecy, France
| | - D A Prokhorov
- Gravitation and Astroparticle Physics at the University of Amsterdam (GRAPPA), Anton Pannekoek Institute for Astronomy, University of Amsterdam, Science Park 904, 1098 XH Amsterdam, Netherlands
| | - H Prokoph
- Deutsches Elektronen-Synchrotron DESY, Platanenallee 6, 15738, Germany
| | - G Pühlhofer
- Institut für Astronomie und Astrophysik, Universität Tübingen, Sand 1, D 72076 Tübingen, Germany
| | - M Punch
- Université de Paris, CNRS, Astroparticule et Cosmologie, F-75013 Paris, France
- Department of Physics and Electrical Engineering, Linnaeus University, 351 95 Växjö, Sweden
| | - A Quirrenbach
- Landessternwarte, Universität Heidelberg, Königstuhl, D 69117 Heidelberg, Germany
| | - P Reichherzer
- Institute for Research on the Fundamental Laws of the Universe (IRFU), Commisariat à l'énergie atomique (CEA), Université Paris-Saclay, F-91191 Gif-sur-Yvette, France
| | - A Reimer
- Institut für Astro- und Teilchenphysik, Leopold-Franzens-Universität Innsbruck, A-6020 Innsbruck, Austria
| | - O Reimer
- Institut für Astro- und Teilchenphysik, Leopold-Franzens-Universität Innsbruck, A-6020 Innsbruck, Austria
| | - M Renaud
- Laboratoire Univers et Particules de Montpellier, Université Montpellier, CNRS/IN2P3, CC 72, Place Eugène Bataillon, F-34095 Montpellier Cedex 5, France
| | - B Reville
- Max-Planck-Institut für Kernphysik, P.O. Box 103980, D 69029 Heidelberg, Germany
| | - F Rieger
- Max-Planck-Institut für Kernphysik, P.O. Box 103980, D 69029 Heidelberg, Germany
| | - G Rowell
- School of Physical Sciences, University of Adelaide, Adelaide 5005, Australia
| | - B Rudak
- Nicolaus Copernicus Astronomical Center, Polish Academy of Sciences, ul. Bartycka 18, 00-716 Warsaw, Poland
| | - H Rueda Ricarte
- Institute for Research on the Fundamental Laws of the Universe (IRFU), Commisariat à l'énergie atomique (CEA), Université Paris-Saclay, F-91191 Gif-sur-Yvette, France
| | - E Ruiz-Velasco
- Max-Planck-Institut für Kernphysik, P.O. Box 103980, D 69029 Heidelberg, Germany
| | - V Sahakian
- Yerevan Physics Institute, 2 Alikhanian Brothers St., 375036 Yerevan, Armenia
| | - S Sailer
- Max-Planck-Institut für Kernphysik, P.O. Box 103980, D 69029 Heidelberg, Germany
| | - H Salzmann
- Institut für Astronomie und Astrophysik, Universität Tübingen, Sand 1, D 72076 Tübingen, Germany
| | - D A Sanchez
- Université Savoie Mont Blanc, CNRS, Laboratoire d'Annecy de Physique des Particules - IN2P3, 74000 Annecy, France
| | - A Santangelo
- Institut für Astronomie und Astrophysik, Universität Tübingen, Sand 1, D 72076 Tübingen, Germany
| | - M Sasaki
- Friedrich-Alexander-Universität Erlangen-Nürnberg, Erlangen Centre for Astroparticle Physics, Erwin-Rommel-Str. 1, D 91058 Erlangen, Germany
| | - J Schäfer
- Friedrich-Alexander-Universität Erlangen-Nürnberg, Erlangen Centre for Astroparticle Physics, Erwin-Rommel-Str. 1, D 91058 Erlangen, Germany
| | - F Schüssler
- Institute for Research on the Fundamental Laws of the Universe (IRFU), Commisariat à l'énergie atomique (CEA), Université Paris-Saclay, F-91191 Gif-sur-Yvette, France
| | - H M Schutte
- Centre for Space Research, North-West University, Potchefstroom 2520, South Africa
| | - U Schwanke
- Institut für Physik, Humboldt-Universität zu Berlin, Newtonstr. 15, D 12489 Berlin, Germany
| | - M Senniappan
- Department of Physics and Electrical Engineering, Linnaeus University, 351 95 Växjö, Sweden
| | - J N S Shapopi
- University of Namibia, Department of Physics, Private Bag 13301, Windhoek 10005, Namibia
| | - R Simoni
- Gravitation and Astroparticle Physics at the University of Amsterdam (GRAPPA), Anton Pannekoek Institute for Astronomy, University of Amsterdam, Science Park 904, 1098 XH Amsterdam, Netherlands
| | - A Sinha
- Laboratoire Univers et Particules de Montpellier, Université Montpellier, CNRS/IN2P3, CC 72, Place Eugène Bataillon, F-34095 Montpellier Cedex 5, France
| | - H Sol
- Laboratoire Univers et Théories, Observatoire de Paris, Université PSL, CNRS, Université de Paris, 92190 Meudon, France
| | - A Specovius
- Friedrich-Alexander-Universität Erlangen-Nürnberg, Erlangen Centre for Astroparticle Physics, Erwin-Rommel-Str. 1, D 91058 Erlangen, Germany
| | - S Spencer
- University of Oxford, Department of Physics, Denys Wilkinson Building, Keble Road, Oxford OX1 3RH, UK
| | - Ł Stawarz
- Obserwatorium Astronomiczne, Uniwersytet Jagielloński, ul. Orla 171, 30-244 Kraków, Poland
| | - S Steinmassl
- Max-Planck-Institut für Kernphysik, P.O. Box 103980, D 69029 Heidelberg, Germany
| | - C Steppa
- Institut für Physik und Astronomie, Universität Potsdam, Karl-Liebknecht-Strasse 24/25, D 14476 Potsdam, Germany
| | - T Takahashi
- Kavli Institute for the Physics and Mathematics of the Universe (World Premier International Research Center Initiative (WPI)), The University of Tokyo Institutes for Advanced Study (UTIAS), The University of Tokyo, 5-1-5 Kashiwa-no-Ha, Kashiwa, Chiba, 277-8583, Japan
| | - T Tanaka
- Department of Physics, Konan University, 8-9-1 Okamoto, Higashinada, Kobe, Hyogo 658-8501, Japan
| | - A M Taylor
- Deutsches Elektronen-Synchrotron DESY, Platanenallee 6, 15738, Germany
| | - R Terrier
- Université de Paris, CNRS, Astroparticule et Cosmologie, F-75013 Paris, France
| | - C Thorpe-Morgan
- Institut für Astronomie und Astrophysik, Universität Tübingen, Sand 1, D 72076 Tübingen, Germany
| | - M Tsirou
- Max-Planck-Institut für Kernphysik, P.O. Box 103980, D 69029 Heidelberg, Germany
| | - N Tsuji
- Institute of Physical and Chemical Research (RIKEN), 2-1 Hirosawa, Wako, Saitama 351-0198, Japan
| | - R Tuffs
- Max-Planck-Institut für Kernphysik, P.O. Box 103980, D 69029 Heidelberg, Germany
| | - Y Uchiyama
- Department of Physics, Rikkyo University, 3-34-1 Nishi-Ikebukuro, Toshima-ku, Tokyo 171-8501, Japan
| | - T Unbehaun
- Friedrich-Alexander-Universität Erlangen-Nürnberg, Erlangen Centre for Astroparticle Physics, Erwin-Rommel-Str. 1, D 91058 Erlangen, Germany
| | - C van Eldik
- Friedrich-Alexander-Universität Erlangen-Nürnberg, Erlangen Centre for Astroparticle Physics, Erwin-Rommel-Str. 1, D 91058 Erlangen, Germany
| | - B van Soelen
- Department of Physics, University of the Free State, PO Box 339, Bloemfontein 9300, South Africa
| | - J Veh
- Friedrich-Alexander-Universität Erlangen-Nürnberg, Erlangen Centre for Astroparticle Physics, Erwin-Rommel-Str. 1, D 91058 Erlangen, Germany
| | - C Venter
- Centre for Space Research, North-West University, Potchefstroom 2520, South Africa
| | - J Vink
- Gravitation and Astroparticle Physics at the University of Amsterdam (GRAPPA), Anton Pannekoek Institute for Astronomy, University of Amsterdam, Science Park 904, 1098 XH Amsterdam, Netherlands
| | - S J Wagner
- Landessternwarte, Universität Heidelberg, Königstuhl, D 69117 Heidelberg, Germany
| | - F Werner
- Max-Planck-Institut für Kernphysik, P.O. Box 103980, D 69029 Heidelberg, Germany
| | - R White
- Max-Planck-Institut für Kernphysik, P.O. Box 103980, D 69029 Heidelberg, Germany
| | - A Wierzcholska
- Instytut Fizyki J[Formula: see text]drowej Polskiej Akademii Nauk (PAN), ul. Radzikowskiego 152, 31-342 Kraków, Poland
| | - Yu Wun Wong
- Friedrich-Alexander-Universität Erlangen-Nürnberg, Erlangen Centre for Astroparticle Physics, Erwin-Rommel-Str. 1, D 91058 Erlangen, Germany
| | - A Yusafzai
- Friedrich-Alexander-Universität Erlangen-Nürnberg, Erlangen Centre for Astroparticle Physics, Erwin-Rommel-Str. 1, D 91058 Erlangen, Germany
| | - M Zacharias
- Centre for Space Research, North-West University, Potchefstroom 2520, South Africa
- Laboratoire Univers et Théories, Observatoire de Paris, Université PSL, CNRS, Université de Paris, 92190 Meudon, France
| | - D Zargaryan
- Dublin Institute for Advanced Studies, 31 Fitzwilliam Place, Dublin 2, Ireland
- High Energy Astrophysics Laboratory, Russian-Armenian University (RAU), 123 Hovsep Emin St Yerevan 0051, Armenia
| | - A A Zdziarski
- Nicolaus Copernicus Astronomical Center, Polish Academy of Sciences, ul. Bartycka 18, 00-716 Warsaw, Poland
| | - A Zech
- Laboratoire Univers et Théories, Observatoire de Paris, Université PSL, CNRS, Université de Paris, 92190 Meudon, France
| | - S J Zhu
- Deutsches Elektronen-Synchrotron DESY, Platanenallee 6, 15738, Germany
| | - S Zouari
- Université de Paris, CNRS, Astroparticule et Cosmologie, F-75013 Paris, France
| | - N Żywucka
- Centre for Space Research, North-West University, Potchefstroom 2520, South Africa
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18
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Cho W, Choi KY, Seto O. Sterile neutrino dark matter with dipole interaction. Int J Clin Exp Med 2022. [DOI: 10.1103/physrevd.105.015016] [Citation(s) in RCA: 0] [Impact Index Per Article: 0] [Reference Citation Analysis] [Track Full Text] [Journal Information] [Subscribe] [Scholar Register] [Indexed: 11/07/2022]
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19
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Abstract
Global modulation studies with comprehensive numerical models contribute meaningfully to the refinement of very local interstellar spectra (VLISs) for cosmic rays. Modulation of positrons and anti-protons are investigated to establish how the ratio of their intensity, and with respect to electrons and protons, are changing with solar activity. This includes the polarity reversal of the solar magnetic field which creates a 22-year modulation cycle. Modeling illustrates how they are modulated over time and the particle drift they experience which is significant at lower kinetic energy. The VLIS for anti-protons has a peculiar spectral shape in contrast to protons so that the total modulation of anti-protons is awkwardly different to that for protons. We find that the proton-to-anti-proton ratio between 1–2 GeV may change by a factor of 1.5 over a solar cycle and that the intensity for anti-protons may decrease by a factor of ~2 at 100 MeV during this cycle. A composition is presented of VLIS for protons, deuteron, helium isotopes, electrons, and particularly for positrons and anti-protons. Gaining knowledge of their respective 11 and 22 year modulation is useful to interpret observations of low-energy anti-nuclei at the Earth as tests of dark matter annihilation.
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20
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Fornieri O, Gaggero D, Guberman D, Brahimi L, Luque PDLT, Marcowith A. Diffusive origin for the cosmic-ray spectral hardening reveals signatures of a nearby source in the leptons and protons data. Int J Clin Exp Med 2021. [DOI: 10.1103/physrevd.104.103013] [Citation(s) in RCA: 4] [Impact Index Per Article: 1.3] [Reference Citation Analysis] [Track Full Text] [Journal Information] [Subscribe] [Scholar Register] [Indexed: 11/07/2022]
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21
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Abstract
We review numerical methods for simulations of cosmic ray (CR) propagation on galactic and larger scales. We present the development of algorithms designed for phenomenological and self-consistent models of CR propagation in kinetic description based on numerical solutions of the Fokker–Planck equation. The phenomenological models assume a stationary structure of the galactic interstellar medium and incorporate diffusion of particles in physical and momentum space together with advection, spallation, production of secondaries and various radiation mechanisms. The self-consistent propagation models of CRs include the dynamical coupling of the CR population to the thermal plasma. The CR transport equation is discretized and solved numerically together with the set of MHD equations in various approaches treating the CR population as a separate relativistic fluid within the two-fluid approach or as a spectrally resolved population of particles evolving in physical and momentum space. The relevant processes incorporated in self-consistent models include advection, diffusion and streaming propagation as well as adiabatic compression and several radiative loss mechanisms. We discuss, applications of the numerical models for the interpretation of CR data collected by various instruments. We present example models of astrophysical processes influencing galactic evolution such as galactic winds, the amplification of large-scale magnetic fields and instabilities of the interstellar medium.
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22
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Aguilar M, Cavasonza LA, Alpat B, Ambrosi G, Arruda L, Attig N, Barao F, Barrin L, Bartoloni A, Başeğmez-du Pree S, Battiston R, Behlmann M, Beranek B, Berdugo J, Bertucci B, Bindi V, Bollweg K, Borgia B, Boschini MJ, Bourquin M, Bueno EF, Burger J, Burger WJ, Burmeister S, Cai XD, Capell M, Casaus J, Castellini G, Cervelli F, Chang YH, Chen GM, Chen GR, Chen HS, Chen Y, Cheng L, Chou HY, Chouridou S, Choutko V, Chung CH, Clark C, Coignet G, Consolandi C, Contin A, Corti C, Cui Z, Dadzie K, Delgado C, Della Torre S, Demirköz MB, Derome L, Di Falco S, Di Felice V, Díaz C, Dimiccoli F, von Doetinchem P, Dong F, Donnini F, Duranti M, Egorov A, Eline A, Feng J, Fiandrini E, Fisher P, Formato V, Freeman C, Gámez C, García-López RJ, Gargiulo C, Gast H, Gervasi M, Giovacchini F, Gómez-Coral DM, Gong J, Goy C, Grabski V, Grandi D, Graziani M, Haino S, Han KC, Hashmani RK, He ZH, Heber B, Hsieh TH, Hu JY, Incagli M, Jang WY, Jia Y, Jinchi H, Khiali B, Kim GN, Kirn T, Konyushikhin M, Kounina O, Kounine A, Koutsenko V, Krasnopevtsev D, Kuhlman A, Kulemzin A, La Vacca G, Laudi E, Laurenti G, Lazzizzera I, Lebedev A, Lee HT, Lee SC, Li JQ, Li M, Li Q, Li S, Li JH, Li ZH, Liang J, Light C, Lin CH, Lippert T, Liu JH, Liu Z, Lu SQ, Lu YS, Luebelsmeyer K, Luo JZ, Luo X, Machate F, Mañá C, Marín J, Marquardt J, Martin T, Martínez G, Masi N, Maurin D, Medvedeva T, Menchaca-Rocha A, Meng Q, Mikhailov VV, Molero M, Mott P, Mussolin L, Negrete J, Nikonov N, Nozzoli F, Oliva A, Orcinha M, Palermo M, Palmonari F, Paniccia M, Pashnin A, Pauluzzi M, Pensotti S, Phan HD, Plyaskin V, Pohl M, Poluianov S, Qin X, Qu ZY, Quadrani L, Rancoita PG, Rapin D, Conde AR, Robyn E, Rosier-Lees S, Rozhkov A, Rozza D, Sagdeev R, Schael S, von Dratzig AS, Schwering G, Seo ES, Shakfa Z, Shan BS, Siedenburg T, Solano C, Song JW, Song XJ, Sonnabend R, Strigari L, Su T, Sun Q, Sun ZT, Tacconi M, Tang XW, Tang ZC, Tian J, Ting SCC, Ting SM, Tomassetti N, Torsti J, Tüysüz C, Urban T, Usoskin I, Vagelli V, Vainio R, Valencia-Otero M, Valente E, Valtonen E, Vázquez Acosta M, Vecchi M, Velasco M, Vialle JP, Wang CX, Wang L, Wang LQ, Wang NH, Wang QL, Wang S, Wang X, Wang Y, Wang ZM, Wei J, Weng ZL, Wu H, Xiong RQ, Xu W, Yan Q, Yang Y, Yashin II, Yi H, Yu YM, Yu ZQ, Zannoni M, Zhang C, Zhang F, Zhang FZ, Zhang JH, Zhang Z, Zhao F, Zheng C, Zheng ZM, Zhuang HL, Zhukov V, Zichichi A, Zuccon P. Erratum: Properties of a New Group of Cosmic Nuclei: Results from the Alpha Magnetic Spectrometer on Sodium, Aluminum, and Nitrogen [Phys. Rev. Lett. 127, 021101 (2021)]. PHYSICAL REVIEW LETTERS 2021; 127:159901. [PMID: 34678040 DOI: 10.1103/physrevlett.127.159901] [Citation(s) in RCA: 0] [Impact Index Per Article: 0] [Reference Citation Analysis] [Abstract] [Track Full Text] [Subscribe] [Scholar Register] [Received: 08/23/2021] [Indexed: 06/13/2023]
Abstract
This corrects the article DOI: 10.1103/PhysRevLett.127.021101.
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23
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Phan VHM, Schulze F, Mertsch P, Recchia S, Gabici S. Stochastic Fluctuations of Low-Energy Cosmic Rays and the Interpretation of Voyager Data. PHYSICAL REVIEW LETTERS 2021; 127:141101. [PMID: 34652203 DOI: 10.1103/physrevlett.127.141101] [Citation(s) in RCA: 3] [Impact Index Per Article: 1.0] [Reference Citation Analysis] [Abstract] [Track Full Text] [Subscribe] [Scholar Register] [Received: 05/04/2021] [Revised: 06/25/2021] [Accepted: 08/17/2021] [Indexed: 06/13/2023]
Abstract
Data from the Voyager probes have provided us with the first measurement of cosmic ray intensities at MeV energies, an energy range that had previously not been explored. Simple extrapolations of models that fit data at GeV energies, e.g., from AMS-02, however, fail to reproduce the Voyager data in that the predicted intensities are too high. Oftentimes, this discrepancy is addressed by adding a break to the source spectrum or the diffusion coefficient in an ad hoc fashion, with a convincing physical explanation yet to be provided. Here, we argue that the discrete nature of cosmic ray sources, which is usually ignored, is instead a more likely explanation. We model the distribution of intensities expected from a statistical model of discrete sources and show that its expectation value is not representative but has a spectral shape different from that for a typical configuration of sources. The Voyager proton and electron data are however compatible with the median of the intensity distribution.
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Affiliation(s)
- Vo Hong Minh Phan
- Institute for Theoretical Particle Physics and Cosmology (TTK), RWTH Aachen University, Aachen 52056, Germany
- Université de Paris, CNRS, Astroparticule et Cosmologie, Paris F-75006, France
| | - Florian Schulze
- Institute for Theoretical Particle Physics and Cosmology (TTK), RWTH Aachen University, Aachen 52056, Germany
| | - Philipp Mertsch
- Institute for Theoretical Particle Physics and Cosmology (TTK), RWTH Aachen University, Aachen 52056, Germany
| | - Sarah Recchia
- Dipartimento di Fisica, Universitá di Torino, via P. Giuria 1, Torino 10125, Italy
| | - Stefano Gabici
- Université de Paris, CNRS, Astroparticule et Cosmologie, Paris F-75006, France
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24
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Boschini MJ, Della Torre S, Gervasi M, Grandi D, Jóhannesson G, La Vacca G, Masi N, Moskalenko IV, Pensotti S, Porter TA, Quadrani L, Rancoita PG, Rozza D, Tacconi M. The Discovery of a Low-energy Excess in Cosmic-Ray Iron: Evidence of the Past Supernova Activity in the Local Bubble. THE ASTROPHYSICAL JOURNAL 2021; 913:5. [PMID: 34646050 PMCID: PMC8506974 DOI: 10.3847/1538-4357/abf11c] [Citation(s) in RCA: 1] [Impact Index Per Article: 0.3] [Reference Citation Analysis] [Abstract] [Key Words] [Grants] [Track Full Text] [Subscribe] [Scholar Register] [Indexed: 06/12/2023]
Abstract
Since its launch, the Alpha Magnetic Spectrometer-02 (AMS-02) has delivered outstanding quality measurements of the spectra of cosmic-ray (CR) species ( p ¯ , e ±, and nuclei, 1H-8O, 10Ne, 12Mg, 14Si) which resulted in a number of breakthroughs. One of the latest long-awaited surprises is the spectrum of 26Fe just published by AMS-02. Because of the large fragmentation cross section and large ionization energy losses, most of CR iron at low energies is local and may harbor some features associated with relatively recent supernova (SN) activity in the solar neighborhood. Our analysis of the new AMS-02 results, together with Voyager 1 and ACE-CRIS data, reveals an unexpected bump in the iron spectrum and in the Fe/He, Fe/O, and Fe/Si ratios at 1-2 GV, while a similar feature in the spectra of He, O, and Si and in their ratios is absent, hinting at a local source of low-energy CRs. The found excess extends the recent discoveries of radioactive 60Fe deposits in terrestrial and lunar samples and in CRs. We provide an updated local interstellar spectrum (LIS) of iron in the energy range from 1 MeV nucleon-1 to ~10 TeV nucleon-1. Our calculations employ the GALPROP-HELMOD framework, which has proved to be a reliable tool in deriving the LIS of CR p ¯ , e -, and nuclei Z ⩽ 28.
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Affiliation(s)
- M J Boschini
- INFN, Milano-Bicocca, Milano, Italy
- CINECA, Segrate, Milano, Italy
| | | | - M Gervasi
- INFN, Milano-Bicocca, Milano, Italy
- Physics Department, University of Milano-Bicocca, Milano, Italy
| | - D Grandi
- INFN, Milano-Bicocca, Milano, Italy
- Physics Department, University of Milano-Bicocca, Milano, Italy
| | - G Jóhannesson
- Science Institute, University of Iceland, Dunhaga 3, IS-107 Reykjavik, Iceland
- NORDITA, Roslagstullsbacken 23, SE-106 91 Stockholm, Sweden
| | - G La Vacca
- INFN, Milano-Bicocca, Milano, Italy
- Physics Department, University of Milano-Bicocca, Milano, Italy
| | - N Masi
- INFN, Bologna, Italy
- Physics Department, University of Bologna, Bologna, Italy
| | - I V Moskalenko
- Hansen Experimental Physics Laboratory, Stanford University, Stanford, CA 94305, USA
- Kavli Institute for Particle Astrophysics and Cosmology, Stanford University, Stanford, CA 94305, USA
| | - S Pensotti
- INFN, Milano-Bicocca, Milano, Italy
- Physics Department, University of Milano-Bicocca, Milano, Italy
| | - T A Porter
- Hansen Experimental Physics Laboratory, Stanford University, Stanford, CA 94305, USA
- Kavli Institute for Particle Astrophysics and Cosmology, Stanford University, Stanford, CA 94305, USA
| | - L Quadrani
- INFN, Bologna, Italy
- Physics Department, University of Bologna, Bologna, Italy
| | | | - D Rozza
- INFN, Milano-Bicocca, Milano, Italy
| | - M Tacconi
- INFN, Milano-Bicocca, Milano, Italy
- Physics Department, University of Milano-Bicocca, Milano, Italy
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25
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Abstract
Continuum gamma-ray emission produced by interactions of cosmic rays with interstellar matter and radiation fields is a probe of non-thermal particle populations in galaxies. After decades of continuous improvements in experimental techniques and an ever-increasing sky and energy coverage, gamma-ray observations reveal in unprecedented detail the properties of galactic cosmic rays. A variety of scales and environments are now accessible to us, from the local interstellar medium near the Sun and the vicinity of cosmic-ray accelerators, out to the Milky Way at large and beyond, with a growing number of gamma-ray emitting star-forming galaxies. Gamma-ray observations have been pushing forward our understanding of the life cycle of cosmic rays in galaxies and, combined with advances in related domains, they have been challenging standard assumptions in the field and have spurred new developments in modelling approaches and data analysis methods. We provide a review of the status of the subject and discuss perspectives on future progress.
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26
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Harnik R, Plestid R, Pospelov M, Ramani H. Millicharged cosmic rays and low recoil detectors. Int J Clin Exp Med 2021. [DOI: 10.1103/physrevd.103.075029] [Citation(s) in RCA: 12] [Impact Index Per Article: 4.0] [Reference Citation Analysis] [Track Full Text] [Journal Information] [Subscribe] [Scholar Register] [Indexed: 11/07/2022]
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27
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Malkov MA, Moskalenko IV. The TeV Cosmic-Ray Bump: A Message from the Epsilon Indi or Epsilon Eridani Star? THE ASTROPHYSICAL JOURNAL 2021; 911:151. [PMID: 34646049 PMCID: PMC8506973 DOI: 10.3847/1538-4357/abe855] [Citation(s) in RCA: 1] [Impact Index Per Article: 0.3] [Reference Citation Analysis] [Abstract] [Key Words] [Grants] [Track Full Text] [Subscribe] [Scholar Register] [Indexed: 06/13/2023]
Abstract
A recently observed bump in the cosmic-ray (CR) spectrum from 0.3 to 30 TV is likely caused by a stellar bow shock that reaccelerates preexisting CRs, which further propagate to the Sun along the magnetic field lines. Along their way, these particles generate an Iroshnikov-Kraichnan (I-K) turbulence that controls their propagation and sustains the bump. Ad hoc fitting of the bump shape requires six adjustable parameters. Our model requires none, merely depending on three physical unknowns that we constrain using the fit. These are the shock Mach number, M, its size, l ⊥, and the distance to it, ζ obs. Altogether, they define the bump rigidity R 0. With M ≈ 1.5-1.6 and R 0 ≈ 4.4 TV, the model fits the data with ≈0.08% accuracy. The fit critically requires the I-K spectrum predicted by the model and rules out the alternatives. These attributes of the fit make an accidental agreement highly unlikely. In turn, the R 0 and M derived from the fit impose the distance-size relation on the shock:ζ obs ( pc ) ~ 10 2 l ⊥ ( pc ) . For sufficiently large bow shocks, l ⊥ = 10-3-10-2 pc, we find the distance of ζ obs = 3-10 pc. Three promising stars in this range are the Scholz's Star at 6.8 pc, Epsilon Indi at 3.6 pc, and Epsilon Eridani at 3.2 pc. Based on their current positions and velocities, we propose that Epsilon Indi and Epsilon Eridani can produce the observed spectral bump. Moreover, Epsilon Eridani's position is only ~6°.7 off of the magnetic field direction in the solar neighborhood, which also changes the CR arrival direction distribution. Given the proximity of these stars, the bump appearance may change in a relatively short time.
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Affiliation(s)
- Mikhail A Malkov
- Department of Physics and CASS, University of California, San Diego, La Jolla, CA 92093, USA
| | - Igor V Moskalenko
- Hansen Experimental Physics Laboratory and Kavli Institute for Particle Astrophysics and Cosmology, Stanford University, Stanford, CA 94305, USA
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28
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Ge SF, Liu J, Yuan Q, Zhou N. Diurnal Effect of Sub-GeV Dark Matter Boosted by Cosmic Rays. PHYSICAL REVIEW LETTERS 2021; 126:091804. [PMID: 33750163 DOI: 10.1103/physrevlett.126.091804] [Citation(s) in RCA: 1] [Impact Index Per Article: 0.3] [Reference Citation Analysis] [Abstract] [Track Full Text] [Subscribe] [Scholar Register] [Received: 05/28/2020] [Accepted: 01/15/2021] [Indexed: 06/12/2023]
Abstract
We point out a new type of diurnal effect for the cosmic ray boosted dark matter (DM). The DM-nucleon interactions not only allow the direct detection of DM with nuclear recoils but also allow cosmic rays to scatter with and boost the nonrelativistic DM to higher energies. If the DM-nuclei scattering cross sections are sufficiently large, the DM flux is attenuated as it propagates through the Earth, leading to a strong diurnal modulation. This diurnal modulation provides another prominent signature for the direct detection of boosted sub-GeV DM, in addition to signals with higher recoil energy.
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Affiliation(s)
- Shao-Feng Ge
- Tsung-Dao Lee Institute, Shanghai Jiao Tong University, Shanghai 200240, China
- School of Physics and Astronomy, Shanghai Jiao Tong University, Key Laboratory for Particle Astrophysics and Cosmology (MOE) and Shanghai Key Laboratory for Particle Physics and Cosmology, Shanghai 200240, China
| | - Jianglai Liu
- Tsung-Dao Lee Institute, Shanghai Jiao Tong University, Shanghai 200240, China
- School of Physics and Astronomy, Shanghai Jiao Tong University, Key Laboratory for Particle Astrophysics and Cosmology (MOE) and Shanghai Key Laboratory for Particle Physics and Cosmology, Shanghai 200240, China
| | - Qiang Yuan
- Key Laboratory of Dark Matter and Space Astronomy, Purple Mountain Observatory, Chinese Academy of Sciences, Nanjing 210033, China
- School of Astronomy and Space Science, University of Science and Technology of China, Hefei 230026, China
- Center for High Energy Physics, Peking University, Beijing 100871, China
| | - Ning Zhou
- School of Physics and Astronomy, Shanghai Jiao Tong University, Key Laboratory for Particle Astrophysics and Cosmology (MOE) and Shanghai Key Laboratory for Particle Physics and Cosmology, Shanghai 200240, China
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29
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Cooper A, Turney CSM, Palmer J, Hogg A, McGlone M, Wilmshurst J, Lorrey AM, Heaton TJ, Russell JM, McCracken K, Anet JG, Rozanov E, Friedel M, Suter I, Peter T, Muscheler R, Adolphi F, Dosseto A, Faith JT, Fenwick P, Fogwill CJ, Hughen K, Lipson M, Liu J, Nowaczyk N, Rainsley E, Bronk Ramsey C, Sebastianelli P, Souilmi Y, Stevenson J, Thomas Z, Tobler R, Zech R. A global environmental crisis 42,000 years ago. Science 2021; 371:811-818. [PMID: 33602851 DOI: 10.1126/science.abb8677] [Citation(s) in RCA: 29] [Impact Index Per Article: 9.7] [Reference Citation Analysis] [Abstract] [Track Full Text] [Journal Information] [Subscribe] [Scholar Register] [Received: 03/24/2020] [Accepted: 12/14/2020] [Indexed: 12/11/2022]
Abstract
Geological archives record multiple reversals of Earth's magnetic poles, but the global impacts of these events, if any, remain unclear. Uncertain radiocarbon calibration has limited investigation of the potential effects of the last major magnetic inversion, known as the Laschamps Excursion [41 to 42 thousand years ago (ka)]. We use ancient New Zealand kauri trees (Agathis australis) to develop a detailed record of atmospheric radiocarbon levels across the Laschamps Excursion. We precisely characterize the geomagnetic reversal and perform global chemistry-climate modeling and detailed radiocarbon dating of paleoenvironmental records to investigate impacts. We find that geomagnetic field minima ~42 ka, in combination with Grand Solar Minima, caused substantial changes in atmospheric ozone concentration and circulation, driving synchronous global climate shifts that caused major environmental changes, extinction events, and transformations in the archaeological record.
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Affiliation(s)
- Alan Cooper
- South Australian Museum, Adelaide, SA 5000, Australia. .,BlueSky Genetics, PO Box 287, Adelaide, SA 5137, Australia
| | - Chris S M Turney
- Chronos Carbon-Cycle Facility, and Earth and Sustainability Science Research Centre, University of New South Wales, Sydney, NSW 2052, Australia.
| | - Jonathan Palmer
- Chronos Carbon-Cycle Facility, and Earth and Sustainability Science Research Centre, University of New South Wales, Sydney, NSW 2052, Australia
| | - Alan Hogg
- Radiocarbon Dating Laboratory, University of Waikato, Hamilton 3240, New Zealand
| | - Matt McGlone
- Landcare Research, PO Box 69040, Lincoln, New Zealand
| | - Janet Wilmshurst
- Landcare Research, PO Box 69040, Lincoln, New Zealand.,School of Environment, University of Auckland, Private Bag 92019, Auckland 1142, New Zealand
| | - Andrew M Lorrey
- National Institute of Water and Atmospheric Research Ltd, Auckland 1010, New Zealand
| | - Timothy J Heaton
- School of Mathematics and Statistics, University of Sheffield, Sheffield S3 7RH, UK
| | - James M Russell
- Department of Geological Sciences, Brown University, Providence, RI 02912, USA
| | - Ken McCracken
- University of New South Wales, Sydney, NSW 2052, Australia
| | - Julien G Anet
- Zurich University of Applied Sciences, Centre for Aviation, 8401 Winterthur, Switzerland
| | - Eugene Rozanov
- Institute for Atmospheric and Climatic Science, ETH Zurich, 8006 Zurich, Switzerland.,Physikalisch-Meteorologisches Observatorium Davos and World Radiation Center, 7260 Davos, Switzerland.,Department of Physics of Earth, Faculty of Physics, St. Petersburg State University, St. Petersburg 198504, Russia
| | - Marina Friedel
- Institute for Atmospheric and Climatic Science, ETH Zurich, 8006 Zurich, Switzerland
| | - Ivo Suter
- Swiss Federal Laboratories for Materials Science and Technology (Empa), 8600 Dübendorf, Switzerland
| | - Thomas Peter
- Institute for Atmospheric and Climatic Science, ETH Zurich, 8006 Zurich, Switzerland
| | - Raimund Muscheler
- Department of Geology, Quaternary Sciences, Lund University, 22362 Lund, Sweden
| | - Florian Adolphi
- Alfred Wegener Institute, Helmholtz Centre for Polar and Marine Research, 27570 Bremerhaven, Germany
| | - Anthony Dosseto
- Wollongong Isotope Geochronology Laboratory, School of Earth, Atmospheric and Life Sciences, University of Wollongong, Wollongong, NSW 2522, Australia
| | - J Tyler Faith
- Natural History Museum of Utah and Department of Anthropology, University of Utah, Salt Lake City, UT 84108, USA
| | - Pavla Fenwick
- Gondwana Tree-Ring Laboratory, PO Box 14, Little River, Canterbury 7546, New Zealand
| | - Christopher J Fogwill
- School of Geography, Geology and the Environment, University of Keele, Keele, Staffordshire ST5 5BG, UK
| | - Konrad Hughen
- Department of Marine Chemistry and Geochemistry, Woods Hole Oceanographic Institution, Woods Hole, MA 02543, USA
| | - Mathew Lipson
- Centre of Excellence for Climate System Science, University of New South Wales, Sydney, NSW 2052, Australia
| | - Jiabo Liu
- Southern University of Science and Technology, Department of Ocean Science and Engineering, Shenzhen 518055, China
| | - Norbert Nowaczyk
- Helmholtz Centre Potsdam, GFZ German Research Centre for Geosciences, Section 4.3, 14473 Potsdam, Germany
| | - Eleanor Rainsley
- School of Geography, Geology and the Environment, University of Keele, Keele, Staffordshire ST5 5BG, UK
| | - Christopher Bronk Ramsey
- Research Laboratory for Archaeology and the History of Art, School of Archaeology, University of Oxford, OX1 3TG, UK
| | - Paolo Sebastianelli
- Faculty of Mathematics, Astronomy and Physics (FAMAF), National University of Cordoba, X5000HUA, Argentina
| | - Yassine Souilmi
- Australian Centre for Ancient DNA, University of Adelaide, Adelaide, SA 5000, Australia
| | - Janelle Stevenson
- Archaeology and Natural History, School of Culture History and Language, ANU College of Asia and the Pacific, Canberra, ACT 2601, Australia.,Australia ARC Centre of Excellence for Australian Biodiversity and Heritage, Australian National University, ACT 2601, Australia
| | - Zoë Thomas
- Chronos Carbon-Cycle Facility, and Earth and Sustainability Science Research Centre, University of New South Wales, Sydney, NSW 2052, Australia
| | - Raymond Tobler
- Australian Centre for Ancient DNA, University of Adelaide, Adelaide, SA 5000, Australia
| | - Roland Zech
- Institute of Geography, Friedrich-Schiller-University Jena, 07743 Jena, Germany
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30
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Boschini MJ, Torre SD, Gervasi M, Grandi D, Jóhannesson G, La Vacca G, Masi N, Moskalenko IV, Pensotti S, Porter TA, Quadrani L, Rancoita PG, Rozza D, Tacconi M. Inference of the Local Interstellar Spectra of Cosmic-Ray Nuclei Z ⩽ 28 with the GalProp-HelMod Framework. THE ASTROPHYSICAL JOURNAL. SUPPLEMENT SERIES 2020; 250:27. [PMID: 34711999 PMCID: PMC8549769 DOI: 10.3847/1538-4365/aba901] [Citation(s) in RCA: 2] [Impact Index Per Article: 0.5] [Reference Citation Analysis] [Abstract] [Key Words] [Grants] [Track Full Text] [Subscribe] [Scholar Register] [Indexed: 05/08/2023]
Abstract
Composition and spectra of Galactic cosmic rays (CRs) are vital for studies of high-energy processes in a variety of environments and on different scales, for interpretation of γ-ray and microwave observations, for disentangling possible signatures of new phenomena, and for understanding of our local Galactic neighborhood. Since its launch, AMS-02 has delivered outstanding-quality measurements of the spectra of p ¯ , e ±, and nuclei: 1H-8O, 10Ne, 12Mg, 14Si. These measurements resulted in a number of breakthroughs; however, spectra of heavier nuclei and especially low-abundance nuclei are not expected until later in the mission. Meanwhile, a comparison of published AMS-02 results with earlier data from HEAO-3-C2 indicates that HEAO-3-C2 data may be affected by undocumented systematic errors. Utilizing such data to compensate for the lack of AMS-02 measurements could result in significant errors. In this paper we show that a fraction of HEAO-3-C2 data match available AMS-02 measurements quite well and can be used together with Voyager 1 and ACE-CRIS data to make predictions for the local interstellar spectra (LIS) of nuclei that are not yet released by AMS-02. We are also updating our already-published LIS to provide a complete set from 1H-28Ni in the energy range from 1 MeV nucleon-1 to ~100-500 TeV nucleon-1, thus covering 8-9 orders of magnitude in energy. Our calculations employ the GalProp-HelMod framework, which has proved to be a reliable tool in deriving the LIS of CR p ¯ , e -, and nuclei 1H-8O.
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Affiliation(s)
- M J Boschini
- INFN, Milano-Bicocca, Milano, Italy
- CINECA, Segrate, Milano, Italy
| | | | - M Gervasi
- INFN, Milano-Bicocca, Milano, Italy
- Physics Department, University of Milano-Bicocca, Milano, Italy
| | - D Grandi
- INFN, Milano-Bicocca, Milano, Italy
- Physics Department, University of Milano-Bicocca, Milano, Italy
| | - G Jóhannesson
- Science Institute, University of Iceland, Dunhaga 3, IS-107 Reykjavik, Iceland
- NORDITA, Roslagstullsbacken 23, 106 91 Stockholm, Sweden
| | - G La Vacca
- INFN, Milano-Bicocca, Milano, Italy
- Physics Department, University of Milano-Bicocca, Milano, Italy
| | - N Masi
- INFN, Bologna, Italy
- Physics Department, University of Bologna, Bologna, Italy
| | - I V Moskalenko
- Hansen Experimental Physics Laboratory, Stanford University, Stanford, CA 94305, USA
- Kavli Institute for Particle Astrophysics and Cosmology, Stanford University, Stanford, CA 94305, USA
| | - S Pensotti
- INFN, Milano-Bicocca, Milano, Italy
- Physics Department, University of Milano-Bicocca, Milano, Italy
| | - T A Porter
- Hansen Experimental Physics Laboratory, Stanford University, Stanford, CA 94305, USA
- Kavli Institute for Particle Astrophysics and Cosmology, Stanford University, Stanford, CA 94305, USA
| | - L Quadrani
- INFN, Bologna, Italy
- Physics Department, University of Bologna, Bologna, Italy
| | | | - D Rozza
- INFN, Milano-Bicocca, Milano, Italy
- Physics Department, University of Milano-Bicocca, Milano, Italy
| | - M Tacconi
- INFN, Milano-Bicocca, Milano, Italy
- Physics Department, University of Milano-Bicocca, Milano, Italy
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31
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Li X, Xiang Z, Zhang K, Khoo L, Zhao H, Baker DN, Temerin MA. New Insights From Long-Term Measurements of Inner Belt Protons (10s of MeV) by SAMPEX, POES, Van Allen Probes, and Simulation Results. JOURNAL OF GEOPHYSICAL RESEARCH. SPACE PHYSICS 2020; 125:e2020JA028198. [PMID: 33042725 PMCID: PMC7539999 DOI: 10.1029/2020ja028198] [Citation(s) in RCA: 0] [Impact Index Per Article: 0] [Reference Citation Analysis] [Abstract] [Key Words] [Grants] [Track Full Text] [Download PDF] [Figures] [Subscribe] [Scholar Register] [Received: 05/06/2020] [Revised: 06/26/2020] [Accepted: 07/21/2020] [Indexed: 06/11/2023]
Abstract
The Solar, Anomalous, and Magnetospheric Particle Explorer (SAMPEX) mission provided long-term measurements of 10s of megaelectron volt (MeV) inner belt (L < 2) protons (1992-2009) as did the Polar-orbiting Operational Environmental Satellite-18 (POES-18, 2005 to present). These long-term measurements at low-Earth orbit (LEO) showed clear solar cycle variations which anticorrelate with sunspot number. However, the magnitude of the variation is much greater than the solar cycle variation of galactic cosmic rays (>GeV) that are regarded as a source of these trapped protons. Furthermore, the proton fluxes and their variations sensitively depend on the altitude above the South Atlantic Anomaly (SAA) region. With respect to protons (>36 MeV) mirroring near the magnetic equator, both POES measurements and simulations show no obvious solar cycle variations at L > 1.2. This is also confirmed by recent measurements from the Van Allen Probes (2012-2019), but there are clear solar cycle variations and a strong spatial gradient of the proton flux below L = 1.2. A direct comparison between measurements and simulations leads to the conclusion that energy loss of trapped protons due to collisions with free and bound electrons in the ionosphere and atmosphere is the dominant mechanism for the strong spatial gradient and solar cycle variation of the inner belt protons. This fact is also key of importance for spacecraft and instrument design and operation in near-Earth space.
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Affiliation(s)
- Xinlin Li
- Laboratory for Atmospheric and Space PhysicsUniversity of Colorado BoulderBoulderCOUSA
- Department of Aerospace Engineering SciencesUniversity of Colorado BoulderBoulderCOUSA
| | - Zheng Xiang
- Laboratory for Atmospheric and Space PhysicsUniversity of Colorado BoulderBoulderCOUSA
- Department of Space Physics, School of Electronic InformationWuhan UniversityWuhanChina
| | - Kun Zhang
- Laboratory for Atmospheric and Space PhysicsUniversity of Colorado BoulderBoulderCOUSA
- Department of Aerospace Engineering SciencesUniversity of Colorado BoulderBoulderCOUSA
| | - Lengying Khoo
- Laboratory for Atmospheric and Space PhysicsUniversity of Colorado BoulderBoulderCOUSA
- Department of Aerospace Engineering SciencesUniversity of Colorado BoulderBoulderCOUSA
| | - Hong Zhao
- Laboratory for Atmospheric and Space PhysicsUniversity of Colorado BoulderBoulderCOUSA
| | - Daniel N. Baker
- Laboratory for Atmospheric and Space PhysicsUniversity of Colorado BoulderBoulderCOUSA
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32
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Cosmic-Ray Database Update: Ultra-High Energy, Ultra-Heavy, and Antinuclei Cosmic-Ray Data (CRDB v4.0). UNIVERSE 2020. [DOI: 10.3390/universe6080102] [Citation(s) in RCA: 16] [Impact Index Per Article: 4.0] [Reference Citation Analysis] [Abstract] [Track Full Text] [Subscribe] [Scholar Register] [Indexed: 11/16/2022]
Abstract
We present an update on CRDB, the cosmic-ray database for charged species. CRDB is based on MySQL, queried and sorted by jquery and table-sorter libraries, and displayed via PHP web pages through the AJAX protocol. We review the modifications made on the structure and outputs of the database since the first release (Maurin et al., 2014). For this update, the most important feature is the inclusion of ultra-heavy nuclei (Z>30), ultra-high energy nuclei (from 1015 to 1020 eV), and limits on antinuclei fluxes (Z≤−1 for A>1); more than 100 experiments, 350 publications, and 40,000 data points are now available in CRDB. We also revisited and simplified how users can retrieve data and submit new ones. For questions and requests, please contact crdb@lpsc.in2p3.fr.
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33
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Cucinotta FA, Cacao E. Predictions of cognitive detriments from galactic cosmic ray exposures to astronauts on exploration missions. LIFE SCIENCES IN SPACE RESEARCH 2020; 25:129-135. [PMID: 32414486 DOI: 10.1016/j.lssr.2019.10.004] [Citation(s) in RCA: 12] [Impact Index Per Article: 3.0] [Reference Citation Analysis] [Abstract] [Key Words] [MESH Headings] [Track Full Text] [Subscribe] [Scholar Register] [Received: 08/25/2019] [Revised: 10/09/2019] [Accepted: 10/13/2019] [Indexed: 06/11/2023]
Abstract
For the first-time we report on predictions on cognitive detriments from galactic cosmic ray (GCR) exposures on long-duration space missions outside the protection of the Earth's magnetosphere and solid body shielding. Estimates are based on a relative risk (RR) model of the fluence response for proton and heavy ion in rodent studies using the widely used novel object recognition (NOR) test, which estimates detriments in recognition or object memory. Our recent meta-analysis showed that linear and linear-quadratic dose response models were not accurate, while exponential increasing fluence response models based on particle track structure provided good descriptions of rodent data for doses up to 1 Gy. Using detailed models of the GCR environment and particle transport in shielding and tissue, we predict the excess relative risk (ERR) for NOR detriments for several long-term space mission scenarios. Predictions suggest ERR < 0.15 for most space mission scenarios with ERR<0.1 for 1-year lunar surface missions, and about ERR~0.1 for a 1000 day Mars mission for average solar cycle conditions. We discuss possible implications of these ERR levels of cognitive performance detriments relative to other neurological challenges such as rodent models of Alzheimer's disease (AD), Parkinson's disease (PD) and traumatic brain injury (TBI). Comparisons suggest a small but potentially clinically significant risk for possible space mission scenarios.
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Affiliation(s)
- Francis A Cucinotta
- Department of Health Physics and Diagnostic Sciences, University of Nevada, Box 453037, Las Vegas, NV 89195-3037, United States.
| | - Eliedonna Cacao
- Department of Health Physics and Diagnostic Sciences, University of Nevada, Box 453037, Las Vegas, NV 89195-3037, United States
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34
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Boschini MJ, Della Torre S, Gervasi M, Grandi D, Jøhannesson G, La Vacca G, Masi N, Moskalenko IV, Pensotti S, Porter TA, Quadrani L, Rancoita PG, Rozza D, Tacconi M. Deciphering the Local Interstellar Spectra of Secondary Nuclei with the Galprop/Helmod Framework and a Hint for Primary Lithium in Cosmic Rays. THE ASTROPHYSICAL JOURNAL 2020; 889:167. [PMID: 34646048 PMCID: PMC8506946 DOI: 10.3847/1538-4357/ab64f1] [Citation(s) in RCA: 34] [Impact Index Per Article: 8.5] [Reference Citation Analysis] [Abstract] [Key Words] [Grants] [Track Full Text] [Subscribe] [Scholar Register] [Indexed: 11/18/2022]
Abstract
Local interstellar spectra (LIS) of secondary cosmic-ray (CR) nuclei, lithium, beryllium, boron, and partially secondary nitrogen, are derived in the rigidity range from 10 MV to ~200 TV using the most recent experimental results combined with state-of-the-art models for CR propagation in the Galaxy and in the heliosphere. The lithium spectrum appears somewhat flatter at high energies compared to other secondary species, which may imply a primary lithium component. Two propagation packages, GALPROP and HelMod, are combined to provide a single framework that is run to reproduce direct measurements of CR species at different modulation levels, and at both polarities of the solar magnetic field. An iterative maximum-likelihood method is developed that uses GALPROP-predicted LIS as input to HelMod, which provides the modulated spectra for specific time periods of the selected experiments for the model-data comparison. The proposed LIS accommodates the low-energy interstellar spectra measured by Voyager 1, the High Energy Astrophysics Observatory-3 (HEAO-3), and the Cosmic Ray Isotope Spectrometer on board of the Advanced Composition Explorer (ACE/CRIS), as well as the high-energy observations by the Payload for Antimatter Matter Exploration and Light-nuclei Astrophysics (PAMELA), Alpha Magnetic Spectrometer-02 (AMS-02), and earlier experiments that are made deep in the heliosphere. The interstellar and heliospheric propagation parameters derived in this study are consistent with our earlier results for propagation of CR protons, helium, carbon, oxygen, antiprotons, and electrons.
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Affiliation(s)
- M J Boschini
- INFN, Milano-Bicocca, Milano, Italy
- CINECA, Segrate, Milano, Italy
| | | | - M Gervasi
- INFN, Milano-Bicocca, Milano, Italy
- Physics Department, University of Milano-Bicocca, Milano, Italy
| | - D Grandi
- INFN, Milano-Bicocca, Milano, Italy
- Physics Department, University of Milano-Bicocca, Milano, Italy
| | - G Jøhannesson
- Science Institute, University of Iceland, Dunhaga 3, IS-107, Reykjavik, Iceland
- NORDITA, Roslagstullsbacken 23, SE-106 91, Stockholm, Sweden
| | - G La Vacca
- INFN, Milano-Bicocca, Milano, Italy
- Physics Department, University of Milano-Bicocca, Milano, Italy
| | | | - I V Moskalenko
- Hansen Experimental Physics Laboratory, Stanford University, Stanford, CA 94305, USA
- Kavli Institute for Particle Astrophysics and Cosmology, Stanford University, Stanford, CA 94305, USA
| | - S Pensotti
- INFN, Milano-Bicocca, Milano, Italy
- Physics Department, University of Milano-Bicocca, Milano, Italy
| | - T A Porter
- Hansen Experimental Physics Laboratory, Stanford University, Stanford, CA 94305, USA
- Kavli Institute for Particle Astrophysics and Cosmology, Stanford University, Stanford, CA 94305, USA
| | - L Quadrani
- INFN, Bologna, Italy
- Physics Department, University of Bologna, Bologna, Italy
| | | | - D Rozza
- INFN, Milano-Bicocca, Milano, Italy
- Physics Department, University of Milano-Bicocca, Milano, Italy
| | - M Tacconi
- INFN, Milano-Bicocca, Milano, Italy
- Physics Department, University of Milano-Bicocca, Milano, Italy
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35
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Coulomb Explosion of Polycyclic Aromatic Hydrocarbons Induced by Heavy Cosmic Rays: Carbon Chains Production Rates. ACTA ACUST UNITED AC 2019. [DOI: 10.3847/1538-4357/ab584f] [Citation(s) in RCA: 5] [Impact Index Per Article: 1.0] [Reference Citation Analysis] [Track Full Text] [Journal Information] [Subscribe] [Scholar Register] [Indexed: 11/18/2022]
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36
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Laha R. Primordial Black Holes as a Dark Matter Candidate Are Severely Constrained by the Galactic Center 511 keV γ-Ray Line. PHYSICAL REVIEW LETTERS 2019; 123:251101. [PMID: 31922779 DOI: 10.1103/physrevlett.123.251101] [Citation(s) in RCA: 11] [Impact Index Per Article: 2.2] [Reference Citation Analysis] [Abstract] [Track Full Text] [Subscribe] [Scholar Register] [Received: 06/25/2019] [Revised: 10/09/2019] [Indexed: 06/10/2023]
Abstract
We derive the strongest constraint on the fraction of dark matter that can be composed of low mass primordial black holes by using the observation of the Galactic Center 511 keV γ-ray line. Primordial black holes of masses ≲10^{15} kg will evaporate to produce e^{±} pairs. The positrons will lose energy in the Galactic Center, become nonrelativistic, then annihilate with the ambient electrons. We derive robust and conservative bounds by assuming that the rate of positron injection via primordial black hole evaporation is less than what is required to explain the SPI/INTEGRAL observation of the Galactic Center 511 keV γ-ray line. Depending on the primordial black hole mass function and other astrophysical uncertainties, these constraints are the most stringent in the literature and show that primordial black holes contribute to less than 1% of the dark matter density. Our technique also probes part of the mass range which was completely unconstrained by previous studies.
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Affiliation(s)
- Ranjan Laha
- Theoretical Physics Department, CERN, 1211 Geneva 23, Switzerland
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37
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38
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The Origin of Cosmic Rays: How Their Composition Defines Their Sources and Sites and the Processes of Their Mixing, Injection, and Acceleration. ACTA ACUST UNITED AC 2019. [DOI: 10.3847/1538-4365/ab4b58] [Citation(s) in RCA: 9] [Impact Index Per Article: 1.8] [Reference Citation Analysis] [Track Full Text] [Journal Information] [Subscribe] [Scholar Register] [Indexed: 11/18/2022]
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39
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Oka T. H 3+, the ideal probe for in situ measurement of the Galactic cosmic rays. PHILOSOPHICAL TRANSACTIONS. SERIES A, MATHEMATICAL, PHYSICAL, AND ENGINEERING SCIENCES 2019; 377:20180402. [PMID: 31378184 DOI: 10.1098/rsta.2018.0402] [Citation(s) in RCA: 1] [Impact Index Per Article: 0.2] [Reference Citation Analysis] [Abstract] [Key Words] [Track Full Text] [Subscribe] [Scholar Register] [Accepted: 04/01/2019] [Indexed: 05/20/2023]
Abstract
The reason why [Formula: see text] is an ideal probe for in situ measurement of cosmic ray energy density in the Galaxy is discussed. The variation of measured values of cosmic ray ionization rate ζ of H2 since the theoretical prediction by Spitzer & Tomasko (Spitzer & Tomasko 1968 Astrophys. J. 152, 971-986) is reviewed. How the measurements by [Formula: see text] established ζ as of the order of 10-17 s-1 for dense clouds, 10-16 s-1 for diffuse clouds in the Galactic disc, and 10-14 s-1 for warm and diffuse gas in the Galactic centre is discussed. This article is part of a discussion meeting issue 'Advances in hydrogen molecular ions: H3+, H5+ and beyond'.
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Affiliation(s)
- Takeshi Oka
- Department of Astronomy and Astrophysics and Department of Chemistry, The Enrico Fermi Institute, University of Chicago, Chicago, IL 60637, USA
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40
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Karwin CM, Murgia S, Campbell S, Moskalenko IV. Fermi-LAT Observations of γ-Ray Emission toward the Outer Halo of M31. THE ASTROPHYSICAL JOURNAL 2019; 880:95. [PMID: 34711992 PMCID: PMC8549762 DOI: 10.3847/1538-4357/ab2880] [Citation(s) in RCA: 6] [Impact Index Per Article: 1.2] [Reference Citation Analysis] [Abstract] [Key Words] [Grants] [Track Full Text] [Subscribe] [Scholar Register] [Indexed: 05/23/2023]
Abstract
The Andromeda galaxy is the closest spiral galaxy to us and has been the subject of numerous studies. It harbors a massive dark matter halo, which may span up to ~600 kpc across and comprises ~90% of the galaxy's total mass. This halo size translates into a large diameter of 42° on the sky, for an M31-Milky Way (MW) distance of 785 kpc, but its presumably low surface brightness makes it challenging to detect with γ-ray telescopes. Using 7.6 yr of Fermi Large Area Telescope (Fermi-LAT) observations, we make a detailed study of the γ-ray emission between 1-100 GeV toward M31's outer halo, with a total field radius of 60° centered at M31, and perform an in-depth analysis of the systematic uncertainties related to the observations. We use the cosmic-ray propagation code GALPROP to construct specialized interstellar emission models to characterize the foreground γ-ray emission from the MW, including a self-consistent determination of the isotropic component. We find evidence for an extended excess that appears to be distinct from the conventional MW foreground, having a total radial extension upward of ~120-200 kpc from the center of M31. We discuss plausible interpretations of the excess emission, but emphasize that uncertainties in the MW foreground-and in particular, modeling of the H i-related components-have not been fully explored and may impact the results.
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Affiliation(s)
- Christopher M Karwin
- Department of Physics and Astronomy, University of California, Irvine, CA 92697, USA
| | - Simona Murgia
- Department of Physics and Astronomy, University of California, Irvine, CA 92697, USA
| | - Sheldon Campbell
- Department of Physics and Astronomy, University of California, Irvine, CA 92697, USA
| | - Igor V Moskalenko
- Hansen Experimental Physics Laboratory and Kavli Institute for Particle Astrophysics and Cosmology, Stanford University, Stanford, CA 94305, USA
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41
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Jóhannesson G, Porter TA, Moskalenko IV. Cosmic-Ray Propagation in Light of the Recent Observation of Geminga. THE ASTROPHYSICAL JOURNAL 2019; 879:91. [PMID: 34646046 PMCID: PMC8506903 DOI: 10.3847/1538-4357/ab258e] [Citation(s) in RCA: 3] [Impact Index Per Article: 0.6] [Reference Citation Analysis] [Abstract] [Key Words] [Grants] [Track Full Text] [Subscribe] [Scholar Register] [Indexed: 05/23/2023]
Abstract
The High Altitude Water Cherenkov (HAWC) telescope recently observed extended emission around the Geminga and PSR B0656+14 pulsar wind nebulae (PWNe). These observations have been used to estimate cosmic-ray (CR) diffusion coefficients near the PWNe that appear to be more than two orders of magnitude smaller than the diffusion coefficients typically derived for the interstellar medium from measured abundances of secondary species in CRs. Two-zone diffusion models have been proposed as a solution to this discrepancy, where the slower diffusion zone (SDZ) is confined to a small region around the PWN. Such models are shown to successfully reproduce the HAWC observations of the Geminga PWN while retaining consistency with other CR data. It is found that the size of the SDZ influences the predicted positron flux and the spectral shape of the extended γ-ray emission at lower energies that can be observed with the Fermi Large Area Telescope. If the two observed PWNe are not unique, then it is likely that there are similar pockets of slow diffusion around many CR sources elsewhere in the Milky Way. The consequences of such a picture for Galactic CR propagation is explored.
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Affiliation(s)
- Guđlaugur Jóhannesson
- Science Institute, University of Iceland, IS-107 Reykjavik, Iceland
- Nordita, KTH Royal Institute of Technology and Stockholm University, Roslagstullsbacken 23, SE-106 91 Stockholm, Sweden
| | - Troy A Porter
- W. W. Hansen Experimental Physics Laboratory and Kavli Institute for Particle Astrophysics and Cosmology, Stanford University, Stanford, CA 94305, USA
| | - Igor V Moskalenko
- W. W. Hansen Experimental Physics Laboratory and Kavli Institute for Particle Astrophysics and Cosmology, Stanford University, Stanford, CA 94305, USA
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42
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Cucinotta FA, Cacao E. Risks of cognitive detriments after low dose heavy ion and proton exposures. Int J Radiat Biol 2019; 95:985-998. [PMID: 31120359 PMCID: PMC6606350 DOI: 10.1080/09553002.2019.1623427] [Citation(s) in RCA: 29] [Impact Index Per Article: 5.8] [Reference Citation Analysis] [Abstract] [Key Words] [MESH Headings] [Grants] [Track Full Text] [Journal Information] [Subscribe] [Scholar Register] [Received: 03/05/2019] [Revised: 04/16/2019] [Accepted: 04/25/2019] [Indexed: 12/15/2022]
Abstract
Purpose: Heavy ion and proton brain irradiations occur during space travel and in Hadron therapy for cancer. Heavy ions produce distinct patterns of energy deposition in neuron cells and brain tissues compared to X-rays leading to large uncertainties in risk estimates. We make a critical review of findings from research studies over the last 25 years for understanding risks at low dose. Conclusions: A large number of mouse and rat cognitive testing measures have been reported for a variety of particle species and energies for acute doses. However, tissue reactions occur above dose thresholds and very few studies were performed at the heavy ion doses to be encountered on space missions (<0.04 Gy/y) or considered dose-rate effects, such that threshold doses are not known in rodent models. Investigations of possible mechanisms for cognitive changes have been limited by experimental design with largely group specific and not subject specific findings reported. Persistent oxidative stress and activated microglia cells are common mechanisms studied, while impairment of neurogenesis, detriments in neuron morphology, and changes to gene and protein expression were each found to be important in specific studies. Future research should focus on estimating threshold doses carried out with experimental designs aimed at understating causative mechanisms, which will be essential for extrapolating rodent findings to humans and chronic radiation scenarios, while establishing if mitigation are needed.
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43
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Shen ZQ, Huang X, Yuan Q, Fan YZ, Wei DM. Probing local cosmic rays using Fermi-LAT observations of a mid-latitude region in the third Galactic quadrant. Int J Clin Exp Med 2019. [DOI: 10.1103/physrevd.99.123001] [Citation(s) in RCA: 2] [Impact Index Per Article: 0.4] [Reference Citation Analysis] [Track Full Text] [Journal Information] [Subscribe] [Scholar Register] [Indexed: 11/07/2022]
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44
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Abstract
We discuss the global modeling of the properties of the Galactic Magnetic Field (GMF). Several improvements and variations of the model of the GMF from Jansson & Farrar (2012) (JF12) are investigated in an analysis constrained by all-sky rotation measures of extragalactic sources and polarized and unpolarized synchrotron emission data from WMAP and Planck. We present the impact of the investigated model variations on the propagation of ultrahigh-energy cosmic rays in the Galaxy
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45
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Abstract
This is a review of the status of efforts to model the large-scale Galactic magnetic field (GMF). Though important for a variety of astrophysical processes, the GMF remains poorly understood despite some interesting new tracers being used in the field. Though we still have too many models that might fit the data, this is not to say that the field has not developed in the last few years. In particular, surveys of polarized dust have given us a new observable that is complementary to the more traditional radio tracers, and a variety of other new tracers and related measurements are becoming available to improve current modeling. This paper reviews: the tracers available; the models that have been studied; what has been learned so far; what the caveats and outstanding issues are; and one opinion of where the most promising future avenues of exploration lie.
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46
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Orlando E. Implications on spatial models of interstellar gamma-ray inverse-Compton emission from synchrotron emission studies in radio and microwaves. Int J Clin Exp Med 2019. [DOI: 10.1103/physrevd.99.043007] [Citation(s) in RCA: 8] [Impact Index Per Article: 1.6] [Reference Citation Analysis] [Track Full Text] [Journal Information] [Subscribe] [Scholar Register] [Indexed: 11/07/2022]
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47
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Boudaud M, Cirelli M. Voyager 1 e^{±} Further Constrain Primordial Black Holes as Dark Matter. PHYSICAL REVIEW LETTERS 2019; 122:041104. [PMID: 30768336 DOI: 10.1103/physrevlett.122.041104] [Citation(s) in RCA: 8] [Impact Index Per Article: 1.6] [Reference Citation Analysis] [Abstract] [Track Full Text] [Subscribe] [Scholar Register] [Received: 07/18/2018] [Revised: 11/26/2018] [Indexed: 06/09/2023]
Abstract
Primordial black holes (PBHs) with a mass M≲10^{17} g are expected to inject sub-GeV electrons and positrons in the Galaxy via Hawking radiation. These cosmic rays are shielded by the solar magnetic field for Earth-bound detectors, but not for Voyager 1, which is now beyond the heliopause. We use its data to constrain the fraction of PBHs to the dark matter in the Galaxy, finding that PBHs with M<10^{16} g cannot contribute more than 0.1% (or less for a log-normal mass distribution). Our limits are based on local Galactic measurements and are thus complementary to those derived from cosmological observations.
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Affiliation(s)
- Mathieu Boudaud
- Laboratoire de Physique Théorique et Hautes Energies (LPTHE), CNRS and Sorbonne Université, 4 Place Jussieu, Paris, France
| | - Marco Cirelli
- Laboratoire de Physique Théorique et Hautes Energies (LPTHE), CNRS and Sorbonne Université, 4 Place Jussieu, Paris, France
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48
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Tomassetti N, Barão F, Bertucci B, Fiandrini E, Figueiredo JL, Lousada JB, Orcinha M. Testing Diffusion of Cosmic Rays in the Heliosphere with Proton and Helium Data from AMS. PHYSICAL REVIEW LETTERS 2018; 121:251104. [PMID: 30608831 DOI: 10.1103/physrevlett.121.251104] [Citation(s) in RCA: 3] [Impact Index Per Article: 0.5] [Reference Citation Analysis] [Abstract] [Track Full Text] [Subscribe] [Scholar Register] [Received: 07/12/2018] [Revised: 09/28/2018] [Indexed: 06/09/2023]
Abstract
After six years of continuous observations in space, the Alpha Magnetic Spectrometer experiment has released new data on the temporal evolution of the proton and helium fluxes in cosmic rays. These data revealed that the ratio between proton and helium fluxes at the same value of rigidity R=p/Z (momentum/charge ratio) is not constant at R≲3 GV. In particular, the ratio is found to decrease steadily during the descending phase of Solar Cycle 24 toward the next minimum. We show that such a behavior is a remarkable signature of the β×λ(R) dependence in the diffusion of cosmic rays in heliosphere, where β is their adimensional speed and λ(R) is their mean free path, a universal function of rigidity for all nuclei. This dependence is responsible for distinctive charge or mass dependent effects in the time-dependent modulation of low-rigidity particles.
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Affiliation(s)
- N Tomassetti
- Università degli Studi di Perugia and INFN-Perugia, I-06100 Perugia, Italy
| | - F Barão
- Laboratório de Instrumentação e Física Experimental de Partículas, P-1000 Lisboa, Portugal
| | - B Bertucci
- Università degli Studi di Perugia and INFN-Perugia, I-06100 Perugia, Italy
| | - E Fiandrini
- Università degli Studi di Perugia and INFN-Perugia, I-06100 Perugia, Italy
| | - J L Figueiredo
- Laboratório de Instrumentação e Física Experimental de Partículas, P-1000 Lisboa, Portugal
| | - J B Lousada
- Laboratório de Instrumentação e Física Experimental de Partículas, P-1000 Lisboa, Portugal
| | - M Orcinha
- Laboratório de Instrumentação e Física Experimental de Partículas, P-1000 Lisboa, Portugal
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49
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Silk J. Molecular Ionization Rates and Ultracompact Dark Matter Minihalos. PHYSICAL REVIEW LETTERS 2018; 121:231105. [PMID: 30576202 DOI: 10.1103/physrevlett.121.231105] [Citation(s) in RCA: 0] [Impact Index Per Article: 0] [Reference Citation Analysis] [Abstract] [Track Full Text] [Subscribe] [Scholar Register] [Received: 08/23/2018] [Revised: 10/05/2018] [Indexed: 06/09/2023]
Abstract
Molecular ionization in the central molecular zone of our Galaxy is enhanced over the typical galactic value by an order of magnitude or more. This cannot be easily explained for dense Galactic center molecular complexes in the absence of embedded sources of low energy cosmic rays. We provide such a source in the form of ultracompact minihalos of self-annihilating dark matter for a variety of annihilation channels that depend on the particle mass and model. Such sources are motivated for plausible inflationary power spectrum parameters, and while possibly subdominant in terms of the total dark matter mass within the Galactic bulge, might also account for, or at least not be in tension with, the Fermi Galactic center γ-ray excess.
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Affiliation(s)
- Joseph Silk
- Institut d'Astrophysique, UMR 7095 CNRS, Sorbonne Université, 98bis Boulevard Arago, 75014 Paris, France, Department of Physics and Astronomy, The Johns Hopkins University, Homewood Campus, Baltimore, Maryland 21218, USA, and Beecroft Institute of Particle Astrophysics and Cosmology, Department of Physics, University of Oxford, Oxford OX1 3RH, United Kingdom
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50
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Aguilar M, Ali Cavasonza L, Alpat B, Ambrosi G, Arruda L, Attig N, Aupetit S, Azzarello P, Bachlechner A, Barao F, Barrau A, Barrin L, Bartoloni A, Basara L, Başeğmez-du Pree S, Battarbee M, Battiston R, Becker U, Behlmann M, Beischer B, Berdugo J, Bertucci B, Bindel KF, Bindi V, de Boer W, Bollweg K, Bonnivard V, Borgia B, Boschini MJ, Bourquin M, Bueno EF, Burger J, Cadoux F, Cai XD, Capell M, Caroff S, Casaus J, Castellini G, Cervelli F, Chae MJ, Chang YH, Chen AI, Chen GM, Chen HS, Chen Y, Cheng L, Chou HY, Choumilov E, Choutko V, Chung CH, Clark C, Clavero R, Coignet G, Consolandi C, Contin A, Corti C, Creus W, Crispoltoni M, Cui Z, Dadzie K, Dai YM, Datta A, Delgado C, Della Torre S, Demirköz MB, Derome L, Di Falco S, Dimiccoli F, Díaz C, von Doetinchem P, Dong F, Donnini F, Duranti M, D'Urso D, Egorov A, Eline A, Eronen T, Feng J, Fiandrini E, Fisher P, Formato V, Galaktionov Y, Gallucci G, García-López RJ, Gargiulo C, Gast H, Gebauer I, Gervasi M, Ghelfi A, Giovacchini F, Gómez-Coral DM, Gong J, Goy C, Grabski V, Grandi D, Graziani M, Guo KH, Haino S, Han KC, He ZH, Heil M, Hoffman J, Hsieh TH, Huang H, Huang ZC, Huh C, Incagli M, Ionica M, Jang WY, Jia Y, Jinchi H, Kang SC, Kanishev K, Khiali B, Kim GN, Kim KS, Kirn T, Konak C, Kounina O, Kounine A, Koutsenko V, Kulemzin A, La Vacca G, Laudi E, Laurenti G, Lazzizzera I, Lebedev A, Lee HT, Lee SC, Leluc C, Li HS, Li JQ, Li Q, Li TX, Li ZH, Li ZY, Light C, Lim S, Lin CH, Lipari P, Lippert T, Liu D, Liu H, Lordello VD, Lu SQ, Lu YS, Luebelsmeyer K, Luo F, Luo JZ, Luo X, Lyu SS, Machate F, Mañá C, Marín J, Martin T, Martínez G, Masi N, Maurin D, Menchaca-Rocha A, Meng Q, Mikuni VM, Mo DC, Mott P, Nelson T, Ni JQ, Nikonov N, Nozzoli F, Oliva A, Orcinha M, Palermo M, Palmonari F, Palomares C, Paniccia M, Pauluzzi M, Pensotti S, Perrina C, Phan HD, Picot-Clemente N, Pilo F, Pizzolotto C, Plyaskin V, Pohl M, Poireau V, Popkow A, Quadrani L, Qi XM, Qin X, Qu ZY, Räihä T, Rancoita PG, Rapin D, Ricol JS, Rosier-Lees S, Rozhkov A, Rozza D, Sagdeev R, Schael S, Schmidt SM, Schulz von Dratzig A, Schwering G, Seo ES, Shan BS, Shi JY, Siedenburg T, Son D, Song JW, Tacconi M, Tang XW, Tang ZC, Tescaro D, Ting SCC, Ting SM, Tomassetti N, Torsti J, Türkoğlu C, Urban T, Vagelli V, Valente E, Valtonen E, Vázquez Acosta M, Vecchi M, Velasco M, Vialle JP, Wang LQ, Wang NH, Wang QL, Wang X, Wang XQ, Wang ZX, Wei CC, Weng ZL, Whitman K, Wu H, Wu X, Xiong RQ, Xu W, Yan Q, Yang J, Yang M, Yang Y, Yi H, Yu YJ, Yu ZQ, Zannoni M, Zeissler S, Zhang C, Zhang F, Zhang J, Zhang JH, Zhang SW, Zhang Z, Zheng ZM, Zhuang HL, Zhukov V, Zichichi A, Zimmermann N, Zuccon P. Observation of Fine Time Structures in the Cosmic Proton and Helium Fluxes with the Alpha Magnetic Spectrometer on the International Space Station. PHYSICAL REVIEW LETTERS 2018; 121:051101. [PMID: 30118264 DOI: 10.1103/physrevlett.121.051101] [Citation(s) in RCA: 14] [Impact Index Per Article: 2.3] [Reference Citation Analysis] [Abstract] [Track Full Text] [Subscribe] [Scholar Register] [Received: 11/21/2017] [Revised: 05/09/2018] [Indexed: 06/08/2023]
Abstract
We present the precision measurement from May 2011 to May 2017 (79 Bartels rotations) of the proton fluxes at rigidities from 1 to 60 GV and the helium fluxes from 1.9 to 60 GV based on a total of 1×10^{9} events collected with the Alpha Magnetic Spectrometer aboard the International Space Station. This measurement is in solar cycle 24, which has the solar maximum in April 2014. We observed that, below 40 GV, the proton flux and the helium flux show nearly identical fine structures in both time and relative amplitude. The amplitudes of the flux structures decrease with increasing rigidity and vanish above 40 GV. The amplitudes of the structures are reduced during the time period, which started one year after solar maximum, when the proton and helium fluxes steadily increase. Above ∼3 GV the p/He flux ratio is time independent. We observed that below ∼3 GV the ratio has a long-term decrease coinciding with the period during which the fluxes start to rise.
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Affiliation(s)
- M Aguilar
- Centro de Investigaciones Energéticas, Medioambientales y Tecnológicas (CIEMAT), E-28040 Madrid, Spain
| | - L Ali Cavasonza
- I. Physics Institute and JARA-FAME, RWTH Aachen University, D-52056 Aachen, Germany
| | - B Alpat
- INFN Sezione di Perugia, I-06100 Perugia, Italy
| | - G Ambrosi
- INFN Sezione di Perugia, I-06100 Perugia, Italy
| | - L Arruda
- Laboratório de Instrumentação e Física Experimental de Partículas (LIP), P-1000 Lisboa, Portugal
| | - N Attig
- Jülich Supercomputing Centre and JARA-FAME, Research Centre Jülich, D-52425 Jülich, Germany
| | - S Aupetit
- Laboratoire de Physique Subatomique et de Cosmologie (LPSC), CNRS/IN2P3 and Université Grenoble-Alpes, F-38026 Grenoble, France
| | - P Azzarello
- DPNC, Université de Genève, CH-1211 Genève 4, Switzerland
| | - A Bachlechner
- I. Physics Institute and JARA-FAME, RWTH Aachen University, D-52056 Aachen, Germany
| | - F Barao
- Laboratório de Instrumentação e Física Experimental de Partículas (LIP), P-1000 Lisboa, Portugal
| | - A Barrau
- Laboratoire de Physique Subatomique et de Cosmologie (LPSC), CNRS/IN2P3 and Université Grenoble-Alpes, F-38026 Grenoble, France
| | - L Barrin
- European Organization for Nuclear Research (CERN), CH-1211 Geneva 23, Switzerland
| | | | - L Basara
- INFN TIFPA, I-38123 Povo, Trento, Italy
| | - S Başeğmez-du Pree
- Institute of High Energy Physics (IHEP), Chinese Academy of Sciences, Beijing, 100049, China
| | - M Battarbee
- Space Research Laboratory, Department of Physics and Astronomy, University of Turku, FI-20014 Turku, Finland
| | - R Battiston
- INFN TIFPA, I-38123 Povo, Trento, Italy
- Università di Trento, I-38123 Povo, Trento, Italy
| | - U Becker
- Massachusetts Institute of Technology (MIT), Cambridge, Massachusetts 02139, USA
| | - M Behlmann
- Massachusetts Institute of Technology (MIT), Cambridge, Massachusetts 02139, USA
| | - B Beischer
- I. Physics Institute and JARA-FAME, RWTH Aachen University, D-52056 Aachen, Germany
| | - J Berdugo
- Centro de Investigaciones Energéticas, Medioambientales y Tecnológicas (CIEMAT), E-28040 Madrid, Spain
| | - B Bertucci
- INFN Sezione di Perugia, I-06100 Perugia, Italy
- Università di Perugia, I-06100 Perugia, Italy
| | - K F Bindel
- Institut für Experimentelle Teilchenphysik, Karlsruhe Institute of Technology (KIT), D-76131 Karlsruhe, Germany
| | - V Bindi
- Physics and Astronomy Department, University of Hawaii, Honolulu, Hawaii 96822, USA
| | - W de Boer
- Institut für Experimentelle Teilchenphysik, Karlsruhe Institute of Technology (KIT), D-76131 Karlsruhe, Germany
| | - K Bollweg
- National Aeronautics and Space Administration Johnson Space Center (JSC), Jacobs Engineering, and Business Integra, Houston, Texas 77058, USA
| | - V Bonnivard
- Laboratoire de Physique Subatomique et de Cosmologie (LPSC), CNRS/IN2P3 and Université Grenoble-Alpes, F-38026 Grenoble, France
| | - B Borgia
- INFN Sezione di Roma 1, I-00185 Roma, Italy
- Università di Roma La Sapienza, I-00185 Roma, Italy
| | - M J Boschini
- INFN Sezione di Milano-Bicocca, I-20126 Milano, Italy
| | - M Bourquin
- DPNC, Université de Genève, CH-1211 Genève 4, Switzerland
| | - E F Bueno
- Instituto de Física de São Carlos, Universidade de São Paulo, CP 369, 13560-970, São Carlos, São Paulo, SP, Brazil
| | - J Burger
- Massachusetts Institute of Technology (MIT), Cambridge, Massachusetts 02139, USA
| | - F Cadoux
- DPNC, Université de Genève, CH-1211 Genève 4, Switzerland
| | - X D Cai
- Massachusetts Institute of Technology (MIT), Cambridge, Massachusetts 02139, USA
| | - M Capell
- Massachusetts Institute of Technology (MIT), Cambridge, Massachusetts 02139, USA
| | - S Caroff
- Laboratoire d'Annecy-le-Vieux de Physique des Particules (LAPP), CNRS/IN2P3 and Université Savoie Mont Blanc, F-74941 Annecy-le-Vieux, France
| | - J Casaus
- Centro de Investigaciones Energéticas, Medioambientales y Tecnológicas (CIEMAT), E-28040 Madrid, Spain
| | | | - F Cervelli
- INFN Sezione di Pisa, I-56100 Pisa, Italy
| | - M J Chae
- Department of Physics, Ewha Womans University, Seoul, 120-750, Korea
| | - Y H Chang
- National Central University (NCU), Chung-Li, Tao Yuan, 32054, Taiwan
| | - A I Chen
- Massachusetts Institute of Technology (MIT), Cambridge, Massachusetts 02139, USA
| | - G M Chen
- Institute of High Energy Physics (IHEP), Chinese Academy of Sciences, Beijing, 100049, China
| | - H S Chen
- Institute of High Energy Physics (IHEP), Chinese Academy of Sciences, Beijing, 100049, China
- University of Chinese Academy of Sciences (UCAS), Beijing, 100049, China
| | - Y Chen
- DPNC, Université de Genève, CH-1211 Genève 4, Switzerland
| | - L Cheng
- Shandong University (SDU), Jinan, Shandong, 250100, China
| | - H Y Chou
- National Central University (NCU), Chung-Li, Tao Yuan, 32054, Taiwan
| | - E Choumilov
- Massachusetts Institute of Technology (MIT), Cambridge, Massachusetts 02139, USA
| | - V Choutko
- Massachusetts Institute of Technology (MIT), Cambridge, Massachusetts 02139, USA
| | - C H Chung
- I. Physics Institute and JARA-FAME, RWTH Aachen University, D-52056 Aachen, Germany
| | - C Clark
- National Aeronautics and Space Administration Johnson Space Center (JSC), Jacobs Engineering, and Business Integra, Houston, Texas 77058, USA
| | - R Clavero
- Instituto de Astrofísica de Canarias (IAC), E-38205 La Laguna, and Departamento de Astrofísica, Universidad de La Laguna, E-38206 La Laguna, Tenerife, Spain
| | - G Coignet
- Laboratoire d'Annecy-le-Vieux de Physique des Particules (LAPP), CNRS/IN2P3 and Université Savoie Mont Blanc, F-74941 Annecy-le-Vieux, France
| | - C Consolandi
- Physics and Astronomy Department, University of Hawaii, Honolulu, Hawaii 96822, USA
| | - A Contin
- INFN Sezione di Bologna, I-40126 Bologna, Italy
- Università di Bologna, I-40126 Bologna, Italy
| | - C Corti
- Physics and Astronomy Department, University of Hawaii, Honolulu, Hawaii 96822, USA
| | - W Creus
- Institute of Physics, Academia Sinica, Nankang, Taipei, 11529, Taiwan
| | - M Crispoltoni
- INFN Sezione di Perugia, I-06100 Perugia, Italy
- Università di Perugia, I-06100 Perugia, Italy
| | - Z Cui
- Shandong University (SDU), Jinan, Shandong, 250100, China
| | - K Dadzie
- Massachusetts Institute of Technology (MIT), Cambridge, Massachusetts 02139, USA
| | - Y M Dai
- Institute of Electrical Engineering (IEE), Chinese Academy of Sciences, Beijing, 100190, China
| | - A Datta
- Physics and Astronomy Department, University of Hawaii, Honolulu, Hawaii 96822, USA
| | - C Delgado
- Centro de Investigaciones Energéticas, Medioambientales y Tecnológicas (CIEMAT), E-28040 Madrid, Spain
| | - S Della Torre
- INFN Sezione di Milano-Bicocca, I-20126 Milano, Italy
| | - M B Demirköz
- Department of Physics, Middle East Technical University (METU), 06800 Ankara, Turkey
| | - L Derome
- Laboratoire de Physique Subatomique et de Cosmologie (LPSC), CNRS/IN2P3 and Université Grenoble-Alpes, F-38026 Grenoble, France
| | - S Di Falco
- INFN Sezione di Pisa, I-56100 Pisa, Italy
| | - F Dimiccoli
- INFN TIFPA, I-38123 Povo, Trento, Italy
- Università di Trento, I-38123 Povo, Trento, Italy
| | - C Díaz
- Centro de Investigaciones Energéticas, Medioambientales y Tecnológicas (CIEMAT), E-28040 Madrid, Spain
| | - P von Doetinchem
- Physics and Astronomy Department, University of Hawaii, Honolulu, Hawaii 96822, USA
| | - F Dong
- Southeast University (SEU), Nanjing, 210096, China
| | - F Donnini
- INFN Sezione di Perugia, I-06100 Perugia, Italy
- Università di Perugia, I-06100 Perugia, Italy
| | - M Duranti
- INFN Sezione di Perugia, I-06100 Perugia, Italy
| | - D D'Urso
- INFN Sezione di Perugia, I-06100 Perugia, Italy
| | - A Egorov
- Massachusetts Institute of Technology (MIT), Cambridge, Massachusetts 02139, USA
| | - A Eline
- Massachusetts Institute of Technology (MIT), Cambridge, Massachusetts 02139, USA
| | - T Eronen
- Space Research Laboratory, Department of Physics and Astronomy, University of Turku, FI-20014 Turku, Finland
| | - J Feng
- Massachusetts Institute of Technology (MIT), Cambridge, Massachusetts 02139, USA
| | - E Fiandrini
- INFN Sezione di Perugia, I-06100 Perugia, Italy
- Università di Perugia, I-06100 Perugia, Italy
| | - P Fisher
- Massachusetts Institute of Technology (MIT), Cambridge, Massachusetts 02139, USA
| | - V Formato
- INFN Sezione di Perugia, I-06100 Perugia, Italy
| | - Y Galaktionov
- Massachusetts Institute of Technology (MIT), Cambridge, Massachusetts 02139, USA
| | - G Gallucci
- INFN Sezione di Pisa, I-56100 Pisa, Italy
| | - R J García-López
- Instituto de Astrofísica de Canarias (IAC), E-38205 La Laguna, and Departamento de Astrofísica, Universidad de La Laguna, E-38206 La Laguna, Tenerife, Spain
| | - C Gargiulo
- European Organization for Nuclear Research (CERN), CH-1211 Geneva 23, Switzerland
| | - H Gast
- I. Physics Institute and JARA-FAME, RWTH Aachen University, D-52056 Aachen, Germany
| | - I Gebauer
- Institut für Experimentelle Teilchenphysik, Karlsruhe Institute of Technology (KIT), D-76131 Karlsruhe, Germany
| | - M Gervasi
- INFN Sezione di Milano-Bicocca, I-20126 Milano, Italy
- Università di Milano-Bicocca, I-20126 Milano, Italy
| | - A Ghelfi
- Laboratoire de Physique Subatomique et de Cosmologie (LPSC), CNRS/IN2P3 and Université Grenoble-Alpes, F-38026 Grenoble, France
| | - F Giovacchini
- Centro de Investigaciones Energéticas, Medioambientales y Tecnológicas (CIEMAT), E-28040 Madrid, Spain
| | - D M Gómez-Coral
- Instituto de Física, Universidad Nacional Autónoma de México (UNAM), México, D. F., 01000 Mexico
| | - J Gong
- Southeast University (SEU), Nanjing, 210096, China
| | - C Goy
- Laboratoire d'Annecy-le-Vieux de Physique des Particules (LAPP), CNRS/IN2P3 and Université Savoie Mont Blanc, F-74941 Annecy-le-Vieux, France
| | - V Grabski
- Instituto de Física, Universidad Nacional Autónoma de México (UNAM), México, D. F., 01000 Mexico
| | - D Grandi
- INFN Sezione di Milano-Bicocca, I-20126 Milano, Italy
| | - M Graziani
- Institut für Experimentelle Teilchenphysik, Karlsruhe Institute of Technology (KIT), D-76131 Karlsruhe, Germany
| | - K H Guo
- Sun Yat-Sen University (SYSU), Guangzhou, 510275, China
| | - S Haino
- Institute of Physics, Academia Sinica, Nankang, Taipei, 11529, Taiwan
| | - K C Han
- National Chung-Shan Institute of Science and Technology (NCSIST), Longtan, Tao Yuan, 32546, Taiwan
| | - Z H He
- Sun Yat-Sen University (SYSU), Guangzhou, 510275, China
| | - M Heil
- Massachusetts Institute of Technology (MIT), Cambridge, Massachusetts 02139, USA
| | - J Hoffman
- Physics and Astronomy Department, University of Hawaii, Honolulu, Hawaii 96822, USA
| | - T H Hsieh
- Massachusetts Institute of Technology (MIT), Cambridge, Massachusetts 02139, USA
| | - H Huang
- Institute of Physics, Academia Sinica, Nankang, Taipei, 11529, Taiwan
| | - Z C Huang
- Sun Yat-Sen University (SYSU), Guangzhou, 510275, China
| | - C Huh
- CHEP, Kyungpook National University, 41566 Daegu, Korea
| | - M Incagli
- INFN Sezione di Pisa, I-56100 Pisa, Italy
| | - M Ionica
- INFN Sezione di Perugia, I-06100 Perugia, Italy
| | - W Y Jang
- CHEP, Kyungpook National University, 41566 Daegu, Korea
| | - Yi Jia
- Massachusetts Institute of Technology (MIT), Cambridge, Massachusetts 02139, USA
| | - H Jinchi
- National Chung-Shan Institute of Science and Technology (NCSIST), Longtan, Tao Yuan, 32546, Taiwan
| | - S C Kang
- CHEP, Kyungpook National University, 41566 Daegu, Korea
| | - K Kanishev
- European Organization for Nuclear Research (CERN), CH-1211 Geneva 23, Switzerland
- INFN TIFPA, I-38123 Povo, Trento, Italy
| | - B Khiali
- National Central University (NCU), Chung-Li, Tao Yuan, 32054, Taiwan
| | - G N Kim
- CHEP, Kyungpook National University, 41566 Daegu, Korea
| | - K S Kim
- CHEP, Kyungpook National University, 41566 Daegu, Korea
| | - Th Kirn
- I. Physics Institute and JARA-FAME, RWTH Aachen University, D-52056 Aachen, Germany
| | - C Konak
- Department of Physics, Middle East Technical University (METU), 06800 Ankara, Turkey
| | - O Kounina
- Massachusetts Institute of Technology (MIT), Cambridge, Massachusetts 02139, USA
| | - A Kounine
- Massachusetts Institute of Technology (MIT), Cambridge, Massachusetts 02139, USA
| | - V Koutsenko
- Massachusetts Institute of Technology (MIT), Cambridge, Massachusetts 02139, USA
| | - A Kulemzin
- Massachusetts Institute of Technology (MIT), Cambridge, Massachusetts 02139, USA
| | - G La Vacca
- INFN Sezione di Milano-Bicocca, I-20126 Milano, Italy
- Università di Milano-Bicocca, I-20126 Milano, Italy
| | - E Laudi
- European Organization for Nuclear Research (CERN), CH-1211 Geneva 23, Switzerland
| | - G Laurenti
- INFN Sezione di Bologna, I-40126 Bologna, Italy
| | - I Lazzizzera
- INFN TIFPA, I-38123 Povo, Trento, Italy
- Università di Trento, I-38123 Povo, Trento, Italy
| | - A Lebedev
- Massachusetts Institute of Technology (MIT), Cambridge, Massachusetts 02139, USA
| | - H T Lee
- Academia Sinica Grid Center (ASGC), Nankang, Taipei, 11529, Taiwan
| | - S C Lee
- Institute of Physics, Academia Sinica, Nankang, Taipei, 11529, Taiwan
| | - C Leluc
- DPNC, Université de Genève, CH-1211 Genève 4, Switzerland
| | - H S Li
- National Cheng Kung University, Tainan, 70101, Taiwan
| | - J Q Li
- Southeast University (SEU), Nanjing, 210096, China
| | - Q Li
- Southeast University (SEU), Nanjing, 210096, China
| | - T X Li
- Sun Yat-Sen University (SYSU), Guangzhou, 510275, China
| | - Z H Li
- Institute of High Energy Physics (IHEP), Chinese Academy of Sciences, Beijing, 100049, China
| | - Z Y Li
- Institute of Physics, Academia Sinica, Nankang, Taipei, 11529, Taiwan
| | - C Light
- Physics and Astronomy Department, University of Hawaii, Honolulu, Hawaii 96822, USA
| | - S Lim
- CHEP, Kyungpook National University, 41566 Daegu, Korea
| | - C H Lin
- Institute of Physics, Academia Sinica, Nankang, Taipei, 11529, Taiwan
| | - P Lipari
- INFN Sezione di Roma 1, I-00185 Roma, Italy
| | - T Lippert
- Jülich Supercomputing Centre and JARA-FAME, Research Centre Jülich, D-52425 Jülich, Germany
| | - D Liu
- National Central University (NCU), Chung-Li, Tao Yuan, 32054, Taiwan
| | - Hu Liu
- Massachusetts Institute of Technology (MIT), Cambridge, Massachusetts 02139, USA
| | - V D Lordello
- Instituto de Física de São Carlos, Universidade de São Paulo, CP 369, 13560-970, São Carlos, São Paulo, SP, Brazil
| | - S Q Lu
- Institute of Physics, Academia Sinica, Nankang, Taipei, 11529, Taiwan
| | - Y S Lu
- Institute of High Energy Physics (IHEP), Chinese Academy of Sciences, Beijing, 100049, China
| | - K Luebelsmeyer
- I. Physics Institute and JARA-FAME, RWTH Aachen University, D-52056 Aachen, Germany
| | - F Luo
- Shandong University (SDU), Jinan, Shandong, 250100, China
| | - J Z Luo
- Southeast University (SEU), Nanjing, 210096, China
| | - X Luo
- Physics and Astronomy Department, University of Hawaii, Honolulu, Hawaii 96822, USA
| | - S S Lyu
- Sun Yat-Sen University (SYSU), Guangzhou, 510275, China
| | - F Machate
- I. Physics Institute and JARA-FAME, RWTH Aachen University, D-52056 Aachen, Germany
| | - C Mañá
- Centro de Investigaciones Energéticas, Medioambientales y Tecnológicas (CIEMAT), E-28040 Madrid, Spain
| | - J Marín
- Centro de Investigaciones Energéticas, Medioambientales y Tecnológicas (CIEMAT), E-28040 Madrid, Spain
| | - T Martin
- National Aeronautics and Space Administration Johnson Space Center (JSC), Jacobs Engineering, and Business Integra, Houston, Texas 77058, USA
| | - G Martínez
- Centro de Investigaciones Energéticas, Medioambientales y Tecnológicas (CIEMAT), E-28040 Madrid, Spain
| | - N Masi
- INFN Sezione di Bologna, I-40126 Bologna, Italy
| | - D Maurin
- Laboratoire de Physique Subatomique et de Cosmologie (LPSC), CNRS/IN2P3 and Université Grenoble-Alpes, F-38026 Grenoble, France
| | - A Menchaca-Rocha
- Instituto de Física, Universidad Nacional Autónoma de México (UNAM), México, D. F., 01000 Mexico
| | - Q Meng
- Southeast University (SEU), Nanjing, 210096, China
| | - V M Mikuni
- Instituto de Física de São Carlos, Universidade de São Paulo, CP 369, 13560-970, São Carlos, São Paulo, SP, Brazil
| | - D C Mo
- Sun Yat-Sen University (SYSU), Guangzhou, 510275, China
| | - P Mott
- National Aeronautics and Space Administration Johnson Space Center (JSC), Jacobs Engineering, and Business Integra, Houston, Texas 77058, USA
| | - T Nelson
- Physics and Astronomy Department, University of Hawaii, Honolulu, Hawaii 96822, USA
| | - J Q Ni
- Sun Yat-Sen University (SYSU), Guangzhou, 510275, China
| | - N Nikonov
- I. Physics Institute and JARA-FAME, RWTH Aachen University, D-52056 Aachen, Germany
| | - F Nozzoli
- INFN Sezione di Perugia, I-06100 Perugia, Italy
| | - A Oliva
- Centro de Investigaciones Energéticas, Medioambientales y Tecnológicas (CIEMAT), E-28040 Madrid, Spain
| | - M Orcinha
- Laboratório de Instrumentação e Física Experimental de Partículas (LIP), P-1000 Lisboa, Portugal
| | - M Palermo
- Physics and Astronomy Department, University of Hawaii, Honolulu, Hawaii 96822, USA
| | - F Palmonari
- INFN Sezione di Bologna, I-40126 Bologna, Italy
- Università di Bologna, I-40126 Bologna, Italy
| | - C Palomares
- Centro de Investigaciones Energéticas, Medioambientales y Tecnológicas (CIEMAT), E-28040 Madrid, Spain
| | - M Paniccia
- DPNC, Université de Genève, CH-1211 Genève 4, Switzerland
| | - M Pauluzzi
- INFN Sezione di Perugia, I-06100 Perugia, Italy
- Università di Perugia, I-06100 Perugia, Italy
| | - S Pensotti
- INFN Sezione di Milano-Bicocca, I-20126 Milano, Italy
- Università di Milano-Bicocca, I-20126 Milano, Italy
| | - C Perrina
- DPNC, Université de Genève, CH-1211 Genève 4, Switzerland
| | - H D Phan
- Massachusetts Institute of Technology (MIT), Cambridge, Massachusetts 02139, USA
| | | | - F Pilo
- INFN Sezione di Pisa, I-56100 Pisa, Italy
| | | | - V Plyaskin
- Massachusetts Institute of Technology (MIT), Cambridge, Massachusetts 02139, USA
| | - M Pohl
- DPNC, Université de Genève, CH-1211 Genève 4, Switzerland
| | - V Poireau
- Laboratoire d'Annecy-le-Vieux de Physique des Particules (LAPP), CNRS/IN2P3 and Université Savoie Mont Blanc, F-74941 Annecy-le-Vieux, France
| | - A Popkow
- Physics and Astronomy Department, University of Hawaii, Honolulu, Hawaii 96822, USA
| | - L Quadrani
- INFN Sezione di Bologna, I-40126 Bologna, Italy
- Università di Bologna, I-40126 Bologna, Italy
| | - X M Qi
- Sun Yat-Sen University (SYSU), Guangzhou, 510275, China
| | - X Qin
- Massachusetts Institute of Technology (MIT), Cambridge, Massachusetts 02139, USA
| | - Z Y Qu
- Institute of Physics, Academia Sinica, Nankang, Taipei, 11529, Taiwan
| | - T Räihä
- I. Physics Institute and JARA-FAME, RWTH Aachen University, D-52056 Aachen, Germany
| | - P G Rancoita
- INFN Sezione di Milano-Bicocca, I-20126 Milano, Italy
| | - D Rapin
- DPNC, Université de Genève, CH-1211 Genève 4, Switzerland
| | - J S Ricol
- Laboratoire de Physique Subatomique et de Cosmologie (LPSC), CNRS/IN2P3 and Université Grenoble-Alpes, F-38026 Grenoble, France
| | - S Rosier-Lees
- Laboratoire d'Annecy-le-Vieux de Physique des Particules (LAPP), CNRS/IN2P3 and Université Savoie Mont Blanc, F-74941 Annecy-le-Vieux, France
| | - A Rozhkov
- Massachusetts Institute of Technology (MIT), Cambridge, Massachusetts 02139, USA
| | - D Rozza
- INFN Sezione di Milano-Bicocca, I-20126 Milano, Italy
- Università di Milano-Bicocca, I-20126 Milano, Italy
| | - R Sagdeev
- East-West Center for Space Science, University of Maryland, College Park, Maryland 20742, USA
| | - S Schael
- I. Physics Institute and JARA-FAME, RWTH Aachen University, D-52056 Aachen, Germany
| | - S M Schmidt
- Jülich Supercomputing Centre and JARA-FAME, Research Centre Jülich, D-52425 Jülich, Germany
| | - A Schulz von Dratzig
- I. Physics Institute and JARA-FAME, RWTH Aachen University, D-52056 Aachen, Germany
| | - G Schwering
- I. Physics Institute and JARA-FAME, RWTH Aachen University, D-52056 Aachen, Germany
| | - E S Seo
- IPST, University of Maryland, College Park, Maryland 20742, USA
| | - B S Shan
- Beihang University (BUAA), Beijing, 100191, China
| | - J Y Shi
- Southeast University (SEU), Nanjing, 210096, China
| | - T Siedenburg
- I. Physics Institute and JARA-FAME, RWTH Aachen University, D-52056 Aachen, Germany
| | - D Son
- CHEP, Kyungpook National University, 41566 Daegu, Korea
| | - J W Song
- Shandong University (SDU), Jinan, Shandong, 250100, China
| | - M Tacconi
- INFN Sezione di Milano-Bicocca, I-20126 Milano, Italy
- Università di Milano-Bicocca, I-20126 Milano, Italy
| | - X W Tang
- Institute of High Energy Physics (IHEP), Chinese Academy of Sciences, Beijing, 100049, China
| | - Z C Tang
- Institute of High Energy Physics (IHEP), Chinese Academy of Sciences, Beijing, 100049, China
| | - D Tescaro
- Instituto de Astrofísica de Canarias (IAC), E-38205 La Laguna, and Departamento de Astrofísica, Universidad de La Laguna, E-38206 La Laguna, Tenerife, Spain
| | - Samuel C C Ting
- Massachusetts Institute of Technology (MIT), Cambridge, Massachusetts 02139, USA
- European Organization for Nuclear Research (CERN), CH-1211 Geneva 23, Switzerland
| | - S M Ting
- Massachusetts Institute of Technology (MIT), Cambridge, Massachusetts 02139, USA
| | - N Tomassetti
- INFN Sezione di Perugia, I-06100 Perugia, Italy
- Università di Perugia, I-06100 Perugia, Italy
| | - J Torsti
- Space Research Laboratory, Department of Physics and Astronomy, University of Turku, FI-20014 Turku, Finland
| | - C Türkoğlu
- Department of Physics, Middle East Technical University (METU), 06800 Ankara, Turkey
| | - T Urban
- National Aeronautics and Space Administration Johnson Space Center (JSC), Jacobs Engineering, and Business Integra, Houston, Texas 77058, USA
| | - V Vagelli
- INFN Sezione di Perugia, I-06100 Perugia, Italy
- Università di Perugia, I-06100 Perugia, Italy
| | - E Valente
- INFN Sezione di Roma 1, I-00185 Roma, Italy
- Università di Roma La Sapienza, I-00185 Roma, Italy
| | - E Valtonen
- Space Research Laboratory, Department of Physics and Astronomy, University of Turku, FI-20014 Turku, Finland
| | - M Vázquez Acosta
- Instituto de Astrofísica de Canarias (IAC), E-38205 La Laguna, and Departamento de Astrofísica, Universidad de La Laguna, E-38206 La Laguna, Tenerife, Spain
| | - M Vecchi
- Instituto de Física de São Carlos, Universidade de São Paulo, CP 369, 13560-970, São Carlos, São Paulo, SP, Brazil
| | - M Velasco
- Centro de Investigaciones Energéticas, Medioambientales y Tecnológicas (CIEMAT), E-28040 Madrid, Spain
| | - J P Vialle
- Laboratoire d'Annecy-le-Vieux de Physique des Particules (LAPP), CNRS/IN2P3 and Université Savoie Mont Blanc, F-74941 Annecy-le-Vieux, France
| | - L Q Wang
- Shandong University (SDU), Jinan, Shandong, 250100, China
| | - N H Wang
- Shandong University (SDU), Jinan, Shandong, 250100, China
| | - Q L Wang
- Institute of Electrical Engineering (IEE), Chinese Academy of Sciences, Beijing, 100190, China
| | - X Wang
- Massachusetts Institute of Technology (MIT), Cambridge, Massachusetts 02139, USA
| | - X Q Wang
- Institute of High Energy Physics (IHEP), Chinese Academy of Sciences, Beijing, 100049, China
- University of Chinese Academy of Sciences (UCAS), Beijing, 100049, China
| | - Z X Wang
- Sun Yat-Sen University (SYSU), Guangzhou, 510275, China
| | - C C Wei
- Institute of Physics, Academia Sinica, Nankang, Taipei, 11529, Taiwan
| | - Z L Weng
- Massachusetts Institute of Technology (MIT), Cambridge, Massachusetts 02139, USA
| | - K Whitman
- Physics and Astronomy Department, University of Hawaii, Honolulu, Hawaii 96822, USA
| | - H Wu
- Southeast University (SEU), Nanjing, 210096, China
| | - X Wu
- DPNC, Université de Genève, CH-1211 Genève 4, Switzerland
| | - R Q Xiong
- Southeast University (SEU), Nanjing, 210096, China
| | - W Xu
- Massachusetts Institute of Technology (MIT), Cambridge, Massachusetts 02139, USA
| | - Q Yan
- Massachusetts Institute of Technology (MIT), Cambridge, Massachusetts 02139, USA
| | - J Yang
- Department of Physics, Ewha Womans University, Seoul, 120-750, Korea
| | - M Yang
- Institute of High Energy Physics (IHEP), Chinese Academy of Sciences, Beijing, 100049, China
| | - Y Yang
- National Cheng Kung University, Tainan, 70101, Taiwan
| | - H Yi
- Southeast University (SEU), Nanjing, 210096, China
| | - Y J Yu
- Institute of Electrical Engineering (IEE), Chinese Academy of Sciences, Beijing, 100190, China
| | - Z Q Yu
- Institute of High Energy Physics (IHEP), Chinese Academy of Sciences, Beijing, 100049, China
| | - M Zannoni
- INFN Sezione di Milano-Bicocca, I-20126 Milano, Italy
- Università di Milano-Bicocca, I-20126 Milano, Italy
| | - S Zeissler
- Institut für Experimentelle Teilchenphysik, Karlsruhe Institute of Technology (KIT), D-76131 Karlsruhe, Germany
| | - C Zhang
- Institute of High Energy Physics (IHEP), Chinese Academy of Sciences, Beijing, 100049, China
| | - F Zhang
- Institute of High Energy Physics (IHEP), Chinese Academy of Sciences, Beijing, 100049, China
| | - J Zhang
- Massachusetts Institute of Technology (MIT), Cambridge, Massachusetts 02139, USA
| | - J H Zhang
- Southeast University (SEU), Nanjing, 210096, China
| | - S W Zhang
- Institute of High Energy Physics (IHEP), Chinese Academy of Sciences, Beijing, 100049, China
- University of Chinese Academy of Sciences (UCAS), Beijing, 100049, China
| | - Z Zhang
- Massachusetts Institute of Technology (MIT), Cambridge, Massachusetts 02139, USA
| | - Z M Zheng
- Beihang University (BUAA), Beijing, 100191, China
| | - H L Zhuang
- Institute of High Energy Physics (IHEP), Chinese Academy of Sciences, Beijing, 100049, China
| | - V Zhukov
- I. Physics Institute and JARA-FAME, RWTH Aachen University, D-52056 Aachen, Germany
| | - A Zichichi
- INFN Sezione di Bologna, I-40126 Bologna, Italy
- Università di Bologna, I-40126 Bologna, Italy
| | - N Zimmermann
- I. Physics Institute and JARA-FAME, RWTH Aachen University, D-52056 Aachen, Germany
| | - P Zuccon
- Massachusetts Institute of Technology (MIT), Cambridge, Massachusetts 02139, USA
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