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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, de Nolfo GA, 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, Okuno S, Ormes JF, 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 Spectral Structure of Cosmic-Ray Electrons+Positrons in the TeV Region with CALET on the International Space Station. PHYSICAL REVIEW LETTERS 2023; 131:191001. [PMID: 38000434 DOI: 10.1103/physrevlett.131.191001] [Citation(s) in RCA: 0] [Impact Index Per Article: 0] [Reference Citation Analysis] [Abstract] [Track Full Text] [Subscribe] [Scholar Register] [Received: 06/02/2023] [Revised: 07/31/2023] [Accepted: 10/09/2023] [Indexed: 11/26/2023]
Abstract
Detailed measurements of the spectral structure of cosmic-ray electrons and positrons from 10.6 GeV to 7.5 TeV are presented from over 7 years of observations with the CALorimetric Electron Telescope (CALET) on the International Space Station. The instrument, consisting of a charge detector, an imaging calorimeter, and a total absorption calorimeter with a total depth of 30 radiation lengths at normal incidence and a fine shower imaging capability, is optimized to measure the all-electron spectrum well into the TeV region. Because of the excellent energy resolution (a few percent above 10 GeV) and the outstanding e/p separation (10^{5}), CALET provides optimal performance for a detailed search of structures in the energy spectrum. The analysis uses data up to the end of 2022, and the statistics of observed electron candidates has increased more than 3 times since the last publication in 2018. By adopting an updated boosted decision tree analysis, a sufficient proton rejection power up to 7.5 TeV is achieved, with a residual proton contamination less than 10%. The observed energy spectrum becomes gradually harder in the lower energy region from around 30 GeV, consistently with AMS-02, but from 300 to 600 GeV it is considerably softer than the spectra measured by DAMPE and Fermi-LAT. At high energies, the spectrum presents a sharp break around 1 TeV, with a spectral index change from -3.15 to -3.91, and a broken power law fitting the data in the energy range from 30 GeV to 4.8 TeV better than a single power law with 6.9 sigma significance, which is compatible with the DAMPE results. The break is consistent with the expected effects of radiation loss during the propagation from distant sources (except the highest energy bin). We have fitted the spectrum with a model consistent with the positron flux measured by AMS-02 below 1 TeV and interpreted the electron+positron spectrum with possible contributions from pulsars and nearby sources. Above 4.8 TeV, a possible contribution from known nearby supernova remnants, including Vela, is addressed by an event-by-event analysis providing a higher proton-rejection power than a purely statistical analysis.
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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
- 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
| | - 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
| | - G A de Nolfo
- Heliospheric Physics Laboratory, NASA/GSFC, Greenbelt, Maryland 20771, USA
| | - 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
- Institute of Applied Physics (IFAC), National Research Council (CNR), Via Madonna del Piano, 10, 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
| | - 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 (KOSEN), 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
- Kanagawa University, 3-27-1 Rokkakubashi, Kanagawa, Yokohama, Kanagawa 221-8686, 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
| | - 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
| | - 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
- 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
- Graduate School of Science, Osaka Metropolitan University, Sugimoto, Sumiyoshi, Osaka 558-8585, Japan
- Nambu Yoichiro Institute for Theoretical and Experimental Physics, Osaka Metropolitan University, 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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Implications of W-Boson Mass Anomaly for Atomic Parity Violation. ATOMS 2022. [DOI: 10.3390/atoms10040149] [Citation(s) in RCA: 0] [Impact Index Per Article: 0] [Reference Citation Analysis] [Abstract] [Track Full Text] [Journal Information] [Subscribe] [Scholar Register] [Indexed: 12/13/2022] Open
Abstract
We consider the implications of the recent measurement of the W-boson mass MW=80,433.5±9.4MeV/c2 for atomic parity violation experiments. We show that the change in MW shifts the Standard Model prediction for the 133Cs nuclear weak charge to QW(133Cs)=−73.11(1), i.e., by 8.5σ from its current value, and the proton weak charge by 2.7%. The shift in QW(133Cs) ameliorates the tension between existing determinations of its value and motivates more accurate atomic theory calculations, while the shift in QW(p) inspires next-generation atomic parity violation experiments with hydrogen. Using our revised value for QW(133Cs), we also readjust constraints on parameters of physics beyond the Standard Model. Finally, we reexamine the running of the electroweak coupling for the new W boson mass.
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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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Pulsar Wind Nebulae and Unidentified Galactic Very High Energy Sources. J 2022. [DOI: 10.3390/j5030022] [Citation(s) in RCA: 0] [Impact Index Per Article: 0] [Reference Citation Analysis] [Abstract] [Track Full Text] [Journal Information] [Subscribe] [Scholar Register] [Indexed: 11/16/2022] Open
Abstract
The riddle of the origin of Cosmic Rays (CR) has been an open question for over a century. Gamma ray observations above 100 MeV reveal the sites of cosmic ray acceleration to energies where they are unaffected by solar modulation; recent evidence supports the existence of hadronic acceleration in Supernova Remnants (SNR), as expected in the standard model of cosmic ray acceleration. Nevertheless, the results raise new questions, and no final answer has been provided thus far. Among the suggested possible alternative accelerators in the Very High Energy (VHE) gamma ray sky, pulsar wind nebulae (PWNe, which together with dark matter are the main candidates to explain the local positron excess as well) are the dominant population among known Galactic sources. However, the most numerous population in absolute terms is represented by unidentified sources (~50% of VHE gamma ray sources). The relationship between PWNe and unidentified sources seems very close; in fact, in a PWN, the lifetime of inverse Compton (IC) emitting electrons not only exceeds the lifetime of its progenitor pulsar, but also exceeds the age of the electrons that emit via synchrotron radiation. Therefore, during its evolution, a PWN can remain bright in IC such that its GeV-TeV gamma ray flux remains high for timescales much larger than the lifetimes of the pulsar and the X-ray PWN. In addition, the shell-type remnant of the supernova explosion in which the pulsar was formed has a much shorter lifetime than the electrons responsible for IC emission. Hence, understanding PWNe and VHE unidentified sources is a crucial piece of the solution to the riddle of the origin of cosmic rays. Both theoretical aspects (with particular emphasis on the ancient pulsar wind nebulae scenario) and their observational proofs are discussed in this paper. Specifically, the scientific cases of HESS J1616-508 and HESS J1813-126 are examined in detail.
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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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Akter S, Hafez MG. Collisional positron acoustic soliton and double layer in an unmagnetized plasma having multi-species. Sci Rep 2022; 12:6453. [PMID: 35440746 PMCID: PMC9018898 DOI: 10.1038/s41598-022-10236-6] [Citation(s) in RCA: 1] [Impact Index Per Article: 0.5] [Reference Citation Analysis] [Abstract] [Track Full Text] [Download PDF] [Figures] [Journal Information] [Subscribe] [Scholar Register] [Received: 12/13/2021] [Accepted: 04/04/2022] [Indexed: 12/04/2022] Open
Abstract
This paper explores the head-on collision between two-counter propagating positron acoustic solitons and double layers (DLs) in an unmagnetized collisionless plasma having mobile cold positrons fluid, immobile positive ions and (\documentclass[12pt]{minimal}
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\begin{document}$$r,\;q$$\end{document}r,q)-distributed hot positrons, and hot electrons. By employing the extended Poincaré–Lighthill–Kuo method, the coupled Korteweg–de Vries (KdV), modified KdV (mKdV) and Gardner equations are derived to archive this goal. The effect of dimensionless parameters on the propagation characteristics of interacting KdV solitons (KdVSs), mKdV solitons (mKdVSs), Gardner solitons (GSs) and DLs are examined in detail by considering the limiting cases of (\documentclass[12pt]{minimal}
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\begin{document}$$r,\;q$$\end{document}r,q)-distribution. It is noted that the interaction of GSs and DLs are reported for the first time. The outcomes might be comprehended and beneficial not only in space and astrophysical environments but also in laboratory studies.
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Affiliation(s)
- Shahrina Akter
- Department of Mathematics, Chittagong University of Engineering and Technology, Chattogram, 4349, Bangladesh.,Department of Mathematics, Premier University, Chattogram, Bangladesh
| | - M G Hafez
- Department of Mathematics, Chittagong University of Engineering and Technology, Chattogram, 4349, Bangladesh.
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7
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Radiation of High-Energy Gamma Quanta by Ultrarelativistic Electrons on Nuclei in Strong X-ray Fields. UNIVERSE 2022. [DOI: 10.3390/universe8040218] [Citation(s) in RCA: 3] [Impact Index Per Article: 1.5] [Reference Citation Analysis] [Abstract] [Track Full Text] [Subscribe] [Scholar Register] [Indexed: 12/04/2022]
Abstract
The possibility of radiation of high-energy gamma quanta with energies of the order of 100 GeV by ultrarelativistic electrons on nuclei in strong X-ray fields with intensities up to ∼1027Wcm−2 was theoretically studied. It is shown that this effect can be realized under special experimental conditions in the process of resonant spontaneous bremsstrahlung radiation of ultrarelativistic electrons on nuclei in an external electromagnetic field. These special experimental conditions determine the characteristic energy of the electrons. This characteristic energy should be significantly less than the energy of the initial electrons. Under these conditions, spontaneous gamma quanta are emitted in a narrow cone with energies close to the energy of the initial electrons. Moreover, the resonant differential cross-sections of such processes can exceed the corresponding differential cross-section without an external field by twenty orders of magnitude. The results obtained can explain the occurrence of high-energy gamma quanta near pulsars and magnetars.
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8
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Sinitsyna VY, Sinitsyna VG, Stozhkov YI. Red Dwarfs as Sources of Cosmic Rays. EPJ WEB OF CONFERENCES 2022. [DOI: 10.1051/epjconf/202226011033] [Citation(s) in RCA: 0] [Impact Index Per Article: 0] [Reference Citation Analysis] [Abstract] [Track Full Text] [Journal Information] [Subscribe] [Scholar Register] [Indexed: 11/14/2022] Open
Abstract
The Pamela, Fermi, AMS-02 spectrometer experimental data cannot be explained using the diffusive models of propagation of cosmic-rays accelerated at the supernova shocks and require the existence of nearby sources of cosmic rays at the distances less than one kpc. These sources could explain the growth of the ratio of galactic positrons to electrons with an energy increase, the complex dependence of the exponent of the proton and alpha spectra on the energy, the cosmic ray anomaly component origin. We consider active dwarf stars as possible sources of galactic cosmic rays in the energy range up to ~ 1014 eV. The generation of high-energy cosmic rays should be accompanied by high-energy gamma-ray emission, which may be detected. The TeV gamma-ray emission mostly of flaring type from active red dwarf stars V388 Cas, V547 Cas, V780 Tau, V962 Tau, V1589 Cyg, GJ 3684, GJ 1078 and GL 851.1 was detected recently with SHALON long-term observations. This result confirms that active dwarf stars are also the sources of high-energy galactic cosmic rays.
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9
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Abstract
The physics of the dark Universe goes beyond the standard model (BSM) of fundamental interactions. The now-standard cosmology involves inflation, baryosynthesis and dark matter/energy corresponding to BSM physics. Cosmoparticle physics offers cross disciplinary study of the fundamental relationship of cosmology and particle physics in the combination of its physical, astrophysical and cosmological signatures. Methods of cosmoparticle physics in studies of BSM physics in its relationship with inevitably nonstandard features of dark universe cosmology are discussed. In the context of these methods, such exotic phenomena as primordial black holes, antimatter stars in baryon asymmetrical Universe or multi-charged constituents of nuclear interacting atoms of composite dark matter play the role of sensitive probes for BSM models and their parameters.
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10
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Line-of-shower trigger method to lower energy threshold for GRB detection using LHAASO-WCDA. RADIATION DETECTION TECHNOLOGY AND METHODS 2021. [DOI: 10.1007/s41605-021-00281-6] [Citation(s) in RCA: 0] [Impact Index Per Article: 0] [Reference Citation Analysis] [Track Full Text] [Journal Information] [Subscribe] [Scholar Register] [Indexed: 11/27/2022]
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11
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Abstract
Slightly more than 30 years ago, Whipple detection of the Crab Nebula was the start of Very High Energy gamma-ray astronomy. Since then, gamma-ray observations of this source have continued to provide new surprises and challenges to theories, with the detection of fast variability, pulsed emission up to unexpectedly high energy, and the very recent detection of photons with energy exceeding 1 PeV. In this article, we review the impact of gamma-ray observations on our understanding of this extraordinary accelerator.
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12
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Cold Particle Dark Matter. Symmetry (Basel) 2021. [DOI: 10.3390/sym13101945] [Citation(s) in RCA: 0] [Impact Index Per Article: 0] [Reference Citation Analysis] [Abstract] [Track Full Text] [Journal Information] [Subscribe] [Scholar Register] [Indexed: 11/16/2022] Open
Abstract
Possible dark matter candidates in particle physics span a mass range extending over fifty orders of magnitude. In this review, we consider the range of masses from a few keV to a few hundred TeV, which is relevant for cold particle dark matter. We will consider models where dark matter arises as weakly coupled elementary fields and models where dark matter is a composite state bound by a new strong interaction. Different production mechanisms for dark matter in these models will be described. The landscape of direct and indirect searches for dark matter and some of the resulting constraints on models will be briefly discussed.
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13
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On a Possible Origin of the Gamma-ray Excess around the Galactic Center. Symmetry (Basel) 2021. [DOI: 10.3390/sym13081432] [Citation(s) in RCA: 0] [Impact Index Per Article: 0] [Reference Citation Analysis] [Abstract] [Track Full Text] [Journal Information] [Subscribe] [Scholar Register] [Indexed: 11/16/2022] Open
Abstract
Recent observations of gamma rays with the Fermi Large Area Telescope (LAT) in the direction of the inner galaxy revealed a mysterious excess of GeV. Its intensity is significantly above predictions of the standard model of cosmic rays (CRs) generation and propagation with a peak in the spectrum around a few GeV. Popular interpretations of this excess are that it is due to either spherically distributed annihilating dark matter (DM) or an abnormal population of millisecond pulsars. We suggest an alternative explanation of the excess through the CR interactions with molecular clouds in the Galactic Center (GC) region. We assumed that the excess could be imitated by the emission of molecular clouds with depleted density of CRs with energies below ∼10 GeV inside. A novelty of our work is in detailed elaboration of the depletion mechanism of CRs with the mentioned energies through the “barrier” near the cloud edge formed by the self-excited MHD turbulence. This depletion of CRs inside the clouds may be a reason for the deficit of gamma rays from the Central Molecular Zone (CMZ) at energies below a few GeV. This in turn changes the ratio between various emission components at those energies and may potentially absorb the GeV excess by a simple renormalization of key components.
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14
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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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15
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Evoli C, Amato E, Blasi P, Aloisio R. Galactic factories of cosmic-ray electrons and positrons. Int J Clin Exp Med 2021. [DOI: 10.1103/physrevd.103.083010] [Citation(s) in RCA: 26] [Impact Index Per Article: 8.7] [Reference Citation Analysis] [Track Full Text] [Journal Information] [Subscribe] [Scholar Register] [Indexed: 11/07/2022]
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16
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Abstract
Indirect searches for dark matter are based on detecting an anomalous flux of photons, neutrinos or cosmic-rays produced in annihilations or decays of dark matter candidates gravitationally accumulated in heavy cosmological objects, like galaxies, the Sun or the Earth. Additionally, evidence for dark matter that can also be understood as indirect can be obtained from early universe probes, like fluctuations of the cosmic microwave background temperature, the primordial abundance of light elements or the Hydrogen 21-cm line. The techniques needed to detect these different signatures require very different types of detectors: Air shower arrays, gamma- and X-ray telescopes, neutrino telescopes, radio telescopes or particle detectors in balloons or satellites. While many of these detectors were not originally intended to search for dark matter, they have proven to be unique complementary tools for direct search efforts. In this review we summarize the current status of indirect searches for dark matter, mentioning also the challenges and limitations that these techniques encounter.
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17
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Resonant Effects in a Photoproduction of Ultrarelativistic Electron-Positron Pairs on a Nucleus in the Field of the X-ray Pulsar. UNIVERSE 2020. [DOI: 10.3390/universe6090141] [Citation(s) in RCA: 6] [Impact Index Per Article: 1.5] [Reference Citation Analysis] [Abstract] [Track Full Text] [Subscribe] [Scholar Register] [Indexed: 11/16/2022]
Abstract
The resonant photoproduction of the electron-positron pairs on a nucleus near a surface of the X-ray pulsar was studied theoretically. The main feature of the processes, which are responsible for the formation of the electron-positron fluxes, is a capability to occur in a resonant way in the electromagnetic field of the X-ray pulsar. One of the properties of the resonant case is that the initial process of second order in the fine structure constant in an external field effectively reduces into two successive processes of the first order due to the fact that in the resonant conditions intermediate virtual electron (positron) becomes a real particle. It is shown that the resonances are possible only when the initial gamma quantum energy is more than the threshold energy, which significantly depends on the number of absorbed photons of an external electromagnetic field. Additionally, in the resonant conditions, the energies of the particles depend on the outgoing angle of a positron (channel A) or an electron (channel B). It is shown that the resonant differential cross section has an extremely large magnitude in units αZ2re2. A mechanism to explain the presence of anomalous fluxes of ultrarelativistic positrons near the surface of an X-ray pulsar was proposed.
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18
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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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19
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Abstract
The High Altitude Water Cherenkov (HAWC) Gamma-Ray Observatory, anextensive air shower detector consisting of 300 water Cherenkov tanks located at 4100m in Puebla, Mexico, has been surveying the TeV gamma-ray sky for almost five years. HAWC can observe steady sources, variable sources, transients, which allows for probes of both astrophysical and particle physics phenomena. This includes the production and propagation of cosmic rays, studies of Lorentz invariance violation, and dark matter searches. I will discuss recent HAWC results as well as the future of the observatory.
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20
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Evoli C, Morlino G, Blasi P, Aloisio R. AMS-02 beryllium data and its implication for cosmic ray transport. Int J Clin Exp Med 2020. [DOI: 10.1103/physrevd.101.023013] [Citation(s) in RCA: 47] [Impact Index Per Article: 11.8] [Reference Citation Analysis] [Track Full Text] [Journal Information] [Subscribe] [Scholar Register] [Indexed: 11/07/2022]
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21
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Barrau A, Martineau K, Moulin F, Ngono JF. Dark matter as Planck relics without too exotic hypotheses. Int J Clin Exp Med 2019. [DOI: 10.1103/physrevd.100.123505] [Citation(s) in RCA: 7] [Impact Index Per Article: 1.4] [Reference Citation Analysis] [Track Full Text] [Journal Information] [Subscribe] [Scholar Register] [Indexed: 11/07/2022]
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22
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Liu RY, Yan H, Zhang H. Understanding the Multiwavelength Observation of Geminga's Tev Halo: The Role of Anisotropic Diffusion of Particles. PHYSICAL REVIEW LETTERS 2019; 123:221103. [PMID: 31868424 DOI: 10.1103/physrevlett.123.221103] [Citation(s) in RCA: 0] [Impact Index Per Article: 0] [Reference Citation Analysis] [Abstract] [Track Full Text] [Subscribe] [Scholar Register] [Received: 04/29/2019] [Revised: 09/17/2019] [Indexed: 06/10/2023]
Abstract
In this Letter, we propose that the x-ray and the TeV observations in the vicinity of Geminga can be understood in the framework of anisotropic diffusion of injected electrons or positrons. This interpretation only requires the turbulence in the vicinity of Geminga to be sub-Alfvénic with the local mean magnetic field direction approximately aligned with our line of sight towards Geminga, without invoking extreme conditions for the environment, such as an extremely small diffusion coefficient and a weak magnetic field of submicrogauss as suggested in previous literature.
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Affiliation(s)
- Ruo-Yu Liu
- Deutsches Elektronen Synchrotron (DESY), Platanenallee 6, D-15738 Zeuthen, Germany
- School of Astronomy and Space Science, Nanjing University, Nanjing 210023, China
| | - Huirong Yan
- Deutsches Elektronen Synchrotron (DESY), Platanenallee 6, D-15738 Zeuthen, Germany
- Institut für Physik und Astronomie, Universität Potsdam, D-14476 Potsdam, Germany
| | - Heshou Zhang
- Deutsches Elektronen Synchrotron (DESY), Platanenallee 6, D-15738 Zeuthen, Germany
- Institut für Physik und Astronomie, Universität Potsdam, D-14476 Potsdam, Germany
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23
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Spatial modelling of Cs-137 and Sr-90 fallout after the Fukushima Nuclear Power Plant accident. J Radioanal Nucl Chem 2019. [DOI: 10.1007/s10967-019-06713-4] [Citation(s) in RCA: 3] [Impact Index Per Article: 0.6] [Reference Citation Analysis] [Track Full Text] [Journal Information] [Subscribe] [Scholar Register] [Indexed: 11/26/2022]
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24
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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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25
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GeV Observations of the Extended Pulsar Wind Nebulae Constrain the Pulsar Interpretations of the Cosmic-Ray Positron Excess. ACTA ACUST UNITED AC 2019. [DOI: 10.3847/1538-4357/ab20c9] [Citation(s) in RCA: 23] [Impact Index Per Article: 4.6] [Reference Citation Analysis] [Track Full Text] [Journal Information] [Subscribe] [Scholar Register] [Indexed: 11/18/2022]
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26
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Abstract
For the understanding of the variable, transient and non-thermal universe, unbiased long-term monitoring is crucial. To constrain the emission mechanisms at the highest energies, it is important to characterize the very high energy emission and its correlation with observations at other wavelengths. At very high energies, only a limited number of instruments is available. This article reviews the current status of monitoring of the extra-galactic sky at TeV energies.
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27
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Abstract
We present the results of the analysis of η → e+e−γ and η → e+e− decays. The experimental data were collected in proton-proton collisions at incident proton kinetic energy 1.4 GeV using the WASA detector and the COSY storage ring. We describe the extraction procedure of the η meson transition form factor, based on a sample of around 108 η mesons, and show an attempt to search for physics beyond the Standard Model that led to the setting of an upper limit on the coupling between photons and hypothetical dark bosons. We also provide an estimate of the branching ratio upper limit for the very rare η → e+e− decay.
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28
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Abstract
There is a commonly expressed opinion in the literature, that cosmic-ray (CR) e+ come from a primary source, which could be dark matter or pulsars. In these proceedings we review some evidence to the contrary: namely, that e+ come from secondary production due to CR nuclei scattering on interstellar matter. We show that recent measurements of the total e± flux at E ≲ 3 TeV are in good agreement with the predicted flux of secondary e±, that would be obtained if radiative energy losses during CR propagation do not play an important role. If the agreement between data and secondary prediction is not accidental, then the requirement of negligible radiative energy losses implies a very short propagation time for high energy CRs: tesc ≲. 105 yr at rigidities R ≳ 3 TV. Such short propagation history may imply that a recent, near-by source dominates the CRs at these energies. We review independent evidence for a transition in CR propagation, based on the spectral hardening of primary and secondary nuclei around R ~ 100 GV. The transition rigidity of the nuclei matches the rigidity at which the e+ flux saturates its secondary upper bound.
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29
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Sinitsyna V, Sinitsyna V, Stozhkov Y. Galactic Cosmic Rays: The first detection of TeV gamma-rays from Red Dwarfs. EPJ WEB OF CONFERENCES 2019. [DOI: 10.1051/epjconf/201920814007] [Citation(s) in RCA: 1] [Impact Index Per Article: 0.2] [Reference Citation Analysis] [Abstract] [Track Full Text] [Journal Information] [Subscribe] [Scholar Register] [Indexed: 11/14/2022] Open
Abstract
The present point of view on the sources of cosmic rays in Galaxy considers explosions of supernovae as sources of these particles up to energies of 1017 eV. However, the experimental data obtained with Pamela, Fermi, AMS-02 spectrometers requires the existence of nearby sources of cosmic rays at distances less then 1 kpc from the solar system. These sources could explain such experimental data as the growth of the ratio of galactic positrons to electrons with increasing energy, the complex dependence of the exponent of the proton and alpha spectra from the energy of these particles, the appearance of an anomaly component in cosmic rays. We consider active dwarf stars as possible sources of galactic cosmic rays in the energy range up to 1014 eV. These stars produce powerful stellar flares. The generation of high-energy cosmic rays has to be accompanied by high-energy gamma-ray emission. Here we present the SHALON long-term observation data aimed at searching for gamma-ray emission above 800 GeV from active red dwarf stars. The data obtained during more than 10 years observations of the dwarf stars V962 Tau, V780 Tau, V388 Cas and V1589 Cyg were analyzed. The high-energy gamma-ray emission in the TeV energy range, mostly of the flaring type from the sources mentioned above, was detected. This result confirms that active dwarf stars are also the sources of high-energy galactic cosmic rays.
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30
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Asaoka Y, Adriani O, Akaike Y, Asano K, Bagliesi MG, Berti E, Bigongiari G, Binns WR, Bonechi S, Bongi M, Bruno A, Brogi P, Buckley JH, Cannady N, Castellini G, Checchia C, Cherry ML, Collazuol G, Di Felice V, Ebisawa K, Fuke H, Guzik TG, Hams T, Hasebe N, Hibinov K, Ichimura M, Ioka K, Ishizaki W, Israel MH, Kasahara K, Kataoka J, Kataoka R, Katayose Y, Kato C, Kawanaka N, Kawakubo Y, Kohri K, Krawczynski HS, Krizmanic JF, Lomtadze T, Maestro P, Marrocchesi PS, Messineo AM, Mitchell JW, Miyake S, Moiseev AA, Mori K, Mori M, Mori N, Motz HM, Munakata K, Murakami H, Nakahira S, Nishimura J, De Nolfo GA, Okuno S, Ormes JF, Ozawa S, Pacini L, Palma F, Pal'shin V, Papini P, Penacchioni AV, Rauch BF, Ricciarini SB, Sakai K, Sakamoto T, Sasaki M, Shimizu Y, Shiomi A, Sparvoli R, Spillantini P, Stolzi F, Sugita S, Suh JE, Sulaj A, Takahashi I, Takayanagi M, Takita M, Tamura T, Tateyama N, Terasawa T, Tomida H, Torii S, Tsunesada Y, Uchihori Y, Ueno S, Vannuccini E, Wefel JP, Yamaoka K, Yanagita S, Yoshida A, Yoshida K. The CALorimetric Electron Telescope (CALET) on the International Space Station: Results from the First Two Years of Operation. EPJ WEB OF CONFERENCES 2019. [DOI: 10.1051/epjconf/201920813001] [Citation(s) in RCA: 0] [Impact Index Per Article: 0] [Reference Citation Analysis] [Abstract] [Track Full Text] [Journal Information] [Subscribe] [Scholar Register] [Indexed: 11/14/2022] Open
Abstract
The CALorimetric Electron Telescope (CALET) space experiment, which has been developed by Japan in collaboration with Italy and the United States, is a high-energy astroparticle physics mission on the International Space Station (ISS). The primary goals of the CALET mission include investigation of possible nearby sources of high-energy electrons, detailed study of galactic cosmic-ray acceleration and propagation, and search for dark matter signatures. With a long-term observation onboard the ISS, the CALET experiment measures the flux of cosmic-ray electrons (including positrons) up to 20 TeV, gamma-rays to 10 TeV, and nuclei up to 1,000 TeV based on its charge separation capability from Z = 1 to 40. Since the start of science operation in mid-October, 2015, a continuous observation has been maintained without any major interruptions. The number of triggered events over 10 GeV is nearly 20 million per month. By using the data obtained during the first two-years, here we present a summary of the CALET observations: 1) Electron+positron energy spectrum, 2) Nuclei analysis, 3) Gamma-ray observation with a characterization of the on-orbit performance. The search results for the electromagnetic counterparts of LIGO/Virgo gravitational wave events are also discussed.
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31
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Abstract
The HAWC (High Altitude Water Cherenkov) observatory, located on the slopes of the Sierra Negra volcano in the state of Puebla, Mexico, was designed with the goal of detecting gamma-rays in the Teraelectron- volt energy range. However, most of the air showers that are detected with the observatory, with a rate of ≈ 27 kHz, are of hadronic origin. This makes that, after three years of operations, HAWC has accumulated a very large data set that allows to perform cosmic-ray analysis of high precision. The details of the observatory operation, as well as a selection of recent results in cosmic-ray physics are discussed in this work.
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32
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López-Coto R, Parsons RD, Hinton JA, Giacinti G. Undiscovered Pulsar in the Local Bubble as an Explanation of the Local High Energy Cosmic Ray All-Electron Spectrum. PHYSICAL REVIEW LETTERS 2018; 121:251106. [PMID: 30608860 DOI: 10.1103/physrevlett.121.251106] [Citation(s) in RCA: 1] [Impact Index Per Article: 0.2] [Reference Citation Analysis] [Abstract] [Track Full Text] [Subscribe] [Scholar Register] [Received: 07/13/2018] [Revised: 10/12/2018] [Indexed: 06/09/2023]
Abstract
Cosmic ray electrons and positrons are tracers of particle propagation in the interstellar medium (ISM). A recent measurement performed using the High Energy Stereoscopic System extends the all-electron (electron+positron) spectrum up to 20 TeV, probing very local sources and transport due to the ∼10 kyr cooling time of these particles. An additional key local measurement was the recent estimation of the ISM diffusion coefficient around Geminga performed using the High-Altitude Water Cherenkov Observatory. The inferred diffusion coefficient is much lower than typically assumed values. It has been argued that if this diffusion coefficient is representative of the local ISM, pulsars would not be able to account for the all-electron spectrum measured at Earth. Here we show that a low diffusion coefficient in the local ISM is compatible with a pulsar wind nebula origin of the highest energy electrons, if a so-far-undiscovered pulsar with spin-down power ∼10^{33-34} erg/s exists within 30-80 pc of Earth. The existence of such a pulsar is broadly consistent with the known population and may be detected in near future survey observations.
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Affiliation(s)
- R López-Coto
- INFN and Università di Padova, I-35131 Padova, Italy
- Max-Planck-Institut für Kernphysik, P.O. Box 103980, D-69029 Heidelberg, Germany
| | - R D Parsons
- 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
| | - G Giacinti
- Max-Planck-Institut für Kernphysik, P.O. Box 103980, D-69029 Heidelberg, Germany
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33
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Archer A, Benbow W, Bird R, Brose R, Buchovecky M, Buckley J, Bugaev V, Connolly M, Cui W, Daniel M, Feng Q, Finley J, Fortson L, Furniss A, Gillanders G, Hütten M, Hanna D, Hervet O, Holder J, Hughes G, Humensky T, Johnson C, Kaaret P, Kar P, Kelley-Hoskins N, Kertzman M, Kieda D, Krause M, Krennrich F, Kumar S, Lang M, Lin T, Maier G, McArthur S, Moriarty P, Mukherjee R, O’Brien S, Ong R, Otte A, Petrashyk A, Pohl M, Pueschel E, Quinn J, Ragan K, Reynolds P, Richards G, Roache E, Rulten C, Sadeh I, Santander M, Sembroski G, Staszak D, Sushch I, Wakely S, Wells R, Wilcox P, Wilhelm A, Williams D, Williamson T, Zitzer B. Measurement of cosmic-ray electrons at TeV energies by VERITAS. Int J Clin Exp Med 2018. [DOI: 10.1103/physrevd.98.062004] [Citation(s) in RCA: 20] [Impact Index Per Article: 3.3] [Reference Citation Analysis] [Track Full Text] [Journal Information] [Subscribe] [Scholar Register] [Indexed: 11/07/2022]
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34
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Génolini Y, Maurin D, Moskalenko IV, Unger M. Current status and desired precision of the isotopic production cross sections relevant to astrophysics of cosmic rays: Li, Be, B, C, and N. PHYSICAL REVIEW. C 2018; 98:034611. [PMID: 34646970 PMCID: PMC8506905 DOI: 10.1103/physrevc.98.034611] [Citation(s) in RCA: 44] [Impact Index Per Article: 7.3] [Reference Citation Analysis] [Abstract] [Grants] [Track Full Text] [Subscribe] [Scholar Register] [Indexed: 11/07/2022]
Abstract
The precision of the current generation of cosmic-ray (CR) experiments, such as AMS-02, PAMELA, CALET, and ISS-CREAM, is now reaching ≈1-3% in a wide range in energy per nucleon from GeV/nucleon to multi-TeV/nucleon. Their correct interpretation could potentially lead to discoveries of new physics and subtle effects that were unthinkable just a decade ago. However, a major obstacle in doing so is the current uncertainty in the isotopic production cross sections that can be as high as 20-50% or even larger in some cases. While there is a recently reached consensus in the astrophysics community that new measurements of cross sections are desirable, no attempt to evaluate the importance of particular reaction channels and their required precision has been made yet. It is, however, clear that it is a huge work that requires an incremental approach. The goal of this study is to provide the ranking of the isotopic cross sections contributing to the production of the most astrophysically important CR Li, Be, B, C, and N species. In this paper, we (i) rank the reaction channels by their importance for a production of a particular isotope, (ii) provide comparisons plots between the models and data used, and (iii) evaluate a generic beam time necessary to reach a 3% precision in the production cross sections pertinent to the AMS-02 experiment. This first road map may become a starting point in the planning of new measurement campaigns that could be carried out in several nuclear and/or particle physics facilities around the world. A comprehensive evaluation of other isotopes Z ⩽ 30 will be a subject of follow-up studies.
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Affiliation(s)
- Yoann Génolini
- Service de Physique Théorique, Université Libre de Bruxelles, Boulevard du Triomphe, CP225, 1050 Brussels, Belgium
| | - David Maurin
- LPSC, Université Grenoble-Alpes, CNRS/IN2P3, 53 avenue des Martyrs, 38026 Grenoble, France
| | - Igor V. Moskalenko
- W. W. Hansen Experimental Physics Laboratory and Kavli Institute for Particle Astrophysics and Cosmology, Stanford University, Stanford, California 94305, USA
| | - Michael Unger
- Karlsruhe Institute of Technology, Karlsruhe, Germany
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Two-zone Diffusion of Electrons and Positrons from Geminga Explains the Positron Anomaly. ACTA ACUST UNITED AC 2018. [DOI: 10.3847/1538-4357/aad092] [Citation(s) in RCA: 51] [Impact Index Per Article: 8.5] [Reference Citation Analysis] [Track Full Text] [Journal Information] [Subscribe] [Scholar Register] [Indexed: 11/18/2022]
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36
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Adriani O, Akaike Y, Asano K, Asaoka Y, Bagliesi MG, Berti E, Bigongiari G, Binns WR, Bonechi S, Bongi M, Brogi P, Buckley JH, Cannady N, Castellini G, Checchia C, Cherry ML, Collazuol G, Di Felice V, Ebisawa K, Fuke H, Guzik TG, Hams T, Hareyama M, Hasebe N, Hibino K, Ichimura M, Ioka K, Ishizaki W, Israel MH, Kasahara K, Kataoka J, Kataoka R, Katayose Y, Kato C, Kawanaka N, Kawakubo Y, Kohri K, Krawczynski HS, Krizmanic JF, Lomtadze T, Maestro P, Marrocchesi PS, Messineo AM, Mitchell JW, Miyake S, Moiseev AA, Mori K, Mori M, Mori N, Motz HM, Munakata K, Murakami H, Nakahira S, Nishimura J, de Nolfo GA, Okuno S, Ormes JF, Ozawa S, Pacini L, Palma F, Papini P, Penacchioni AV, Rauch BF, Ricciarini SB, Sakai K, Sakamoto T, Sasaki M, Shimizu Y, Shiomi A, Sparvoli R, Spillantini P, Stolzi F, Suh JE, Sulaj A, Takahashi I, Takayanagi M, Takita M, Tamura T, Tateyama N, Terasawa T, Tomida H, Torii S, Tsunesada Y, Uchihori Y, Ueno S, Vannuccini E, Wefel JP, Yamaoka K, Yanagita S, Yoshida A, Yoshida K. Extended Measurement of the Cosmic-Ray Electron and Positron Spectrum from 11 GeV to 4.8 TeV with the Calorimetric Electron Telescope on the International Space Station. PHYSICAL REVIEW LETTERS 2018; 120:261102. [PMID: 30004739 DOI: 10.1103/physrevlett.120.261102] [Citation(s) in RCA: 13] [Impact Index Per Article: 2.2] [Reference Citation Analysis] [Abstract] [Track Full Text] [Subscribe] [Scholar Register] [Received: 02/16/2018] [Revised: 05/21/2018] [Indexed: 06/08/2023]
Abstract
Extended results on the cosmic-ray electron + positron spectrum from 11 GeV to 4.8 TeV are presented based on observations with the Calorimetric Electron Telescope (CALET) on the International Space Station utilizing the data up to November 2017. The analysis uses the full detector acceptance at high energies, approximately doubling the statistics compared to the previous result. CALET is an all-calorimetric instrument with a total thickness of 30 X_{0} at normal incidence and fine imaging capability, designed to achieve large proton rejection and excellent energy resolution well into the TeV energy region. The observed energy spectrum in the region below 1 TeV shows good agreement with Alpha Magnetic Spectrometer (AMS-02) data. In the energy region below ∼300 GeV, CALET's spectral index is found to be consistent with the AMS-02, Fermi Large Area Telescope (Fermi-LAT), and Dark Matter Particle Explorer (DAMPE), while from 300 to 600 GeV the spectrum is significantly softer than the spectra from the latter two experiments. The absolute flux of CALET is consistent with other experiments at around a few tens of GeV. However, it is lower than those of DAMPE and Fermi-LAT with the difference increasing up to several hundred GeV. The observed energy spectrum above ∼1 TeV suggests a flux suppression consistent within the errors with the results of DAMPE, while CALET does not observe any significant evidence for a narrow spectral feature in the energy region around 1.4 TeV. Our measured all-electron flux, including statistical errors and a detailed breakdown of the systematic errors, is tabulated in the Supplemental Material in order to allow more refined spectral analyses based on our data.
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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
- Department of Physics, University of Maryland, Baltimore County, 1000 Hilltop Circle, Baltimore, Maryland 21250, USA
- Astroparticle Physics Laboratory, NASA/GSFC, Greenbelt, Maryland 20771, USA
| | - K Asano
- Institute for Cosmic Ray Research, The University of Tokyo, 5-1-5 Kashiwa-no-Ha, Kashiwa, Chiba 277-8582, Japan
| | - Y Asaoka
- Research Institute for Science and Engineering, Waseda University, 3-4-1 Okubo, Shinjuku, Tokyo 169-8555, Japan
- JEM Utilization Center, Human Spaceflight Technology Directorate, Japan Aerospace Exploration Agency, 2-1-1 Sengen, Tsukuba, Ibaraki 305-8505, Japan
| | - M G Bagliesi
- 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
| | - 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, Washington University, One Brookings Drive, St. Louis, Missouri 63130-4899, USA
| | - S Bonechi
- 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 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
| | - J H Buckley
- Department of Physics, Washington University, One Brookings Drive, St. Louis, Missouri 63130-4899, USA
| | - N Cannady
- Department of Physics and Astronomy, Louisiana State University, 202 Nicholson Hall, Baton Rouge, Louisiana 70803, 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 Physics and Astronomy, University of Padova, Via Marzolo, 8, 35131 Padova, Italy
- INFN Sezione di Padova, Via Marzolo, 8, 35131 Padova, 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
| | - V Di Felice
- University of Rome "Tor Vergata", Via della Ricerca Scientifica 1, 00133 Rome, Italy
- INFN Sezione di Rome "Tor Vergata", Via della Ricerca Scientifica 1, 00133 Rome, Italy
| | - K Ebisawa
- Institute of Space and Astronautical Science, Japan Aerospace Exploration Agency, 3-1-1 Yoshinodai, Chuo, Sagamihara, Kanagawa 252-5210, Japan
| | - H Fuke
- Institute of Space and Astronautical Science, Japan Aerospace Exploration Agency, 3-1-1 Yoshinodai, Chuo, Sagamihara, Kanagawa 252-5210, Japan
| | - T G Guzik
- Department of Physics and Astronomy, Louisiana State University, 202 Nicholson Hall, Baton Rouge, Louisiana 70803, USA
| | - T Hams
- Department of Physics, University of Maryland, Baltimore County, 1000 Hilltop Circle, Baltimore, Maryland 21250, USA
- CRESST and Astroparticle Physics Laboratory NASA/GSFC, Greenbelt, Maryland 20771, USA
| | - M Hareyama
- St. Marianna University School of Medicine, 2-16-1, Sugao, Miyamae-ku, Kawasaki, Kanagawa 216-8511, Japan
| | - N Hasebe
- Research Institute for Science and Engineering, Waseda University, 3-4-1 Okubo, Shinjuku, Tokyo 169-8555, Japan
| | - 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 Oiwakecho, Sakyo, 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, Washington University, One Brookings Drive, St. Louis, Missouri 63130-4899, USA
| | - K Kasahara
- Research Institute for Science and Engineering, Waseda University, 3-4-1 Okubo, Shinjuku, Tokyo 169-8555, Japan
| | - J Kataoka
- Research Institute for 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
- Hakubi Center, Kyoto University, Yoshida Honmachi, Sakyo-ku, Kyoto 606-8501, Japan
- Department of Astronomy, Graduate School of Science, Kyoto University, Kitashirakawa Oiwake-cho, Sakyo-ku, Kyoto 606-8502, Japan
| | - Y Kawakubo
- College of Science and Engineering, Department of Physics and Mathematics, Aoyama Gakuin University, 5-10-1 Fuchinobe, Chuo, Sagamihara, Kanagawa 252-5258, 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, Washington University, One Brookings Drive, St. Louis, Missouri 63130-4899, USA
| | - J F Krizmanic
- Department of Physics, University of Maryland, Baltimore County, 1000 Hilltop Circle, Baltimore, Maryland 21250, USA
- CRESST and Astroparticle Physics Laboratory NASA/GSFC, Greenbelt, Maryland 20771, USA
| | - T Lomtadze
- INFN Sezione di Pisa, Polo Fibonacci, Largo B. Pontecorvo, 3-56127 Pisa, Italy
| | - 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
- CRESST and Astroparticle Physics Laboratory NASA/GSFC, Greenbelt, Maryland 20771, USA
- Department of Astronomy, University of Maryland, College Park, Maryland 20742, USA
| | - K Mori
- Research Institute for Science and Engineering, Waseda University, 3-4-1 Okubo, Shinjuku, Tokyo 169-8555, Japan
- Institute of Space and Astronautical Science, Japan Aerospace Exploration Agency, 3-1-1 Yoshinodai, Chuo, Sagamihara, Kanagawa 252-5210, Japan
| | - 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
- International Center for Science and Engineering Programs, 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
| | - H Murakami
- Research Institute for Science and Engineering, Waseda University, 3-4-1 Okubo, Shinjuku, Tokyo 169-8555, Japan
| | - S Nakahira
- RIKEN, 2-1 Hirosawa, Wako, Saitama 351-0198, 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
| | - S Ozawa
- Research Institute for Science and Engineering, Waseda University, 3-4-1 Okubo, Shinjuku, Tokyo 169-8555, 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
| | - F Palma
- University of Rome "Tor Vergata", Via della Ricerca Scientifica 1, 00133 Rome, Italy
- INFN Sezione di Rome "Tor Vergata", Via della Ricerca Scientifica 1, 00133 Rome, Italy
| | - P Papini
- INFN Sezione di Florence, Via Sansone, 1-50019 Sesto, Fiorentino, Italy
| | - A V Penacchioni
- Department of Physical Sciences, Earth and Environment, University of Siena, via Roma 56, 53100 Siena, Italy
- ASI Science Data Center (ASDC), Via del Politecnico snc, 00133 Rome, Italy
| | - B F Rauch
- Department of Physics, 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
- Department of Physics, University of Maryland, Baltimore County, 1000 Hilltop Circle, Baltimore, Maryland 21250, USA
- CRESST and Astroparticle Physics Laboratory 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
- CRESST and Astroparticle Physics Laboratory 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
| | - R Sparvoli
- University of Rome "Tor Vergata", Via della Ricerca Scientifica 1, 00133 Rome, Italy
- INFN Sezione di Rome "Tor Vergata", Via della Ricerca Scientifica 1, 00133 Rome, Italy
| | - 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
| | - J E Suh
- 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 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
| | - I Takahashi
- Kavli Institute for the Physics and Mathematics of the Universe, The University of Tokyo, 5-1-5 Kashiwanoha, Kashiwa, 277-8583, Japan
| | - M Takayanagi
- Institute of Space and Astronautical Science, Japan Aerospace Exploration Agency, 3-1-1 Yoshinodai, Chuo, Sagamihara, Kanagawa 252-5210, Japan
| | - 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
| | - N Tateyama
- Kanagawa University, 3-27-1 Rokkakubashi, Kanagawa, Yokohama, Kanagawa 221-8686, Japan
| | - T Terasawa
- RIKEN, 2-1 Hirosawa, Wako, Saitama 351-0198, Japan
| | - H Tomida
- Institute of Space and Astronautical Science, Japan Aerospace Exploration Agency, 3-1-1 Yoshinodai, Chuo, Sagamihara, Kanagawa 252-5210, Japan
| | - S Torii
- Research Institute for Science and Engineering, Waseda University, 3-4-1 Okubo, Shinjuku, Tokyo 169-8555, Japan
- JEM Utilization Center, Human Spaceflight Technology Directorate, Japan Aerospace Exploration Agency, 2-1-1 Sengen, Tsukuba, Ibaraki 305-8505, Japan
- School of Advanced Science and Engineering, Waseda University, 3-4-1 Okubo, Shinjuku, Tokyo 169-8555, Japan
| | - Y Tsunesada
- Division of Mathematics and Physics, Graduate School of Science, 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
| | - S Ueno
- Institute of Space and Astronautical Science, Japan Aerospace Exploration Agency, 3-1-1 Yoshinodai, Chuo, Sagamihara, Kanagawa 252-5210, 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
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Roszkowski L, Sessolo EM, Trojanowski S. WIMP dark matter candidates and searches-current status and future prospects. REPORTS ON PROGRESS IN PHYSICS. PHYSICAL SOCIETY (GREAT BRITAIN) 2018; 81:066201. [PMID: 29569575 DOI: 10.1088/1361-6633/aab913] [Citation(s) in RCA: 16] [Impact Index Per Article: 2.7] [Reference Citation Analysis] [Abstract] [Track Full Text] [Subscribe] [Scholar Register] [Indexed: 06/08/2023]
Abstract
We review several current aspects of dark matter theory and experiment. We overview the present experimental status, which includes current bounds and recent claims and hints of a possible signal in a wide range of experiments: direct detection in underground laboratories, gamma-ray, cosmic ray, x-ray, neutrino telescopes, and the LHC. We briefly review several possible particle candidates for a weakly interactive massive particle (WIMP) and dark matter that have recently been considered in the literature. We pay particular attention to the lightest neutralino of supersymmetry as it remains the best motivated candidate for dark matter and also shows excellent detection prospects. Finally we briefly review some alternative scenarios that can considerably alter properties and prospects for the detection of dark matter obtained within the standard thermal WIMP paradigm.
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Affiliation(s)
- Leszek Roszkowski
- National Centre for Nuclear Research, Hoża 69, 00-681 Warsaw, Poland. Department of Physics and Astronomy, University of Sheffield, Sheffield S3 7RH, United Kingdom
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Korsmeier M, Donato F, Di Mauro M. Production cross sections of cosmic antiprotons in the light of new data from the NA61 and LHCb experiments. Int J Clin Exp Med 2018. [DOI: 10.1103/physrevd.97.103019] [Citation(s) in RCA: 30] [Impact Index Per Article: 5.0] [Reference Citation Analysis] [Track Full Text] [Journal Information] [Subscribe] [Scholar Register] [Indexed: 11/07/2022]
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Cao J, Feng L, Guo X, Shang L, Wang F, Wu P. Scalar dark matter interpretation of the DAMPE data with U(1) gauge interactions. Int J Clin Exp Med 2018. [DOI: 10.1103/physrevd.97.095011] [Citation(s) in RCA: 13] [Impact Index Per Article: 2.2] [Reference Citation Analysis] [Track Full Text] [Journal Information] [Subscribe] [Scholar Register] [Indexed: 11/07/2022]
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Niu JS, Li T, Ding R, Zhu B, Xue HF, Wang Y. Bayesian analysis of the break in
DAMPE
lepton spectra. Int J Clin Exp Med 2018. [DOI: 10.1103/physrevd.97.083012] [Citation(s) in RCA: 17] [Impact Index Per Article: 2.8] [Reference Citation Analysis] [Track Full Text] [Journal Information] [Subscribe] [Scholar Register] [Indexed: 11/07/2022]
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Abeysekara AU, Albert A, Alfaro R, Alvarez C, Álvarez JD, Arceo R, Arteaga-Velázquez JC, Avila Rojas D, Ayala Solares HA, Barber AS, Bautista-Elivar N, Becerril A, Belmont-Moreno E, BenZvi SY, Berley D, Bernal A, Braun J, Brisbois C, Caballero-Mora KS, Capistrán T, Carramiñana A, Casanova S, Castillo M, Cotti U, Cotzomi J, Coutiño de León S, De León C, De la Fuente E, Dingus BL, DuVernois MA, Díaz-Vélez JC, Ellsworth RW, Engel K, Enríquez-Rivera O, Fiorino DW, Fraija N, García-González JA, Garfias F, Gerhardt M, González Muñoz A, González MM, Goodman JA, Hampel-Arias Z, Harding JP, Hernández S, Hernández-Almada A, Hinton J, Hona B, Hui CM, Hüntemeyer P, Iriarte A, Jardin-Blicq A, Joshi V, Kaufmann S, Kieda D, Lara A, Lauer RJ, Lee WH, Lennarz D, Vargas HL, Linnemann JT, Longinotti AL, Luis Raya G, Luna-García R, López-Coto R, Malone K, Marinelli SS, Martinez O, Martinez-Castellanos I, Martínez-Castro J, Martínez-Huerta H, Matthews JA, Miranda-Romagnoli P, Moreno E, Mostafá M, Nellen L, Newbold M, Nisa MU, Noriega-Papaqui R, Pelayo R, Pretz J, Pérez-Pérez EG, Ren Z, Rho CD, Rivière C, Rosa-González D, Rosenberg M, Ruiz-Velasco E, Salazar H, Salesa Greus F, Sandoval A, Schneider M, Schoorlemmer H, Sinnis G, Smith AJ, Springer RW, Surajbali P, Taboada I, Tibolla O, Tollefson K, Torres I, Ukwatta TN, Vianello G, Weisgarber T, Westerhoff S, Wisher IG, Wood J, Yapici T, Yodh G, Younk PW, Zepeda A, Zhou H, Guo F, Hahn J, Li H, Zhang H. Extended gamma-ray sources around pulsars constrain the origin of the positron flux at Earth. Science 2018; 358:911-914. [PMID: 29146808 DOI: 10.1126/science.aan4880] [Citation(s) in RCA: 211] [Impact Index Per Article: 35.2] [Reference Citation Analysis] [Abstract] [Track Full Text] [Journal Information] [Subscribe] [Scholar Register] [Received: 04/20/2017] [Accepted: 10/09/2017] [Indexed: 11/02/2022]
Abstract
The unexpectedly high flux of cosmic-ray positrons detected at Earth may originate from nearby astrophysical sources, dark matter, or unknown processes of cosmic-ray secondary production. We report the detection, using the High-Altitude Water Cherenkov Observatory (HAWC), of extended tera-electron volt gamma-ray emission coincident with the locations of two nearby middle-aged pulsars (Geminga and PSR B0656+14). The HAWC observations demonstrate that these pulsars are indeed local sources of accelerated leptons, but the measured tera-electron volt emission profile constrains the diffusion of particles away from these sources to be much slower than previously assumed. We demonstrate that the leptons emitted by these objects are therefore unlikely to be the origin of the excess positrons, which may have a more exotic origin.
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Affiliation(s)
- A U Abeysekara
- Department of Physics and Astronomy, University of Utah, Salt Lake City, UT, USA
| | - A Albert
- Los Alamos National Laboratory, Los Alamos, NM, USA
| | - R Alfaro
- Instituto de Física, Universidad Nacional Autónoma de México, Mexico City, Mexico
| | - C Alvarez
- Universidad Autónoma de Chiapas, Tuxtla Gutiérrez, Chiapas, Mexico
| | - J D Álvarez
- Universidad Michoacana de San Nicolás de Hidalgo, Morelia, Mexico
| | - R Arceo
- Universidad Autónoma de Chiapas, Tuxtla Gutiérrez, Chiapas, Mexico
| | | | - D Avila Rojas
- Instituto de Física, Universidad Nacional Autónoma de México, Mexico City, Mexico
| | - H A Ayala Solares
- Department of Physics, Michigan Technological University, Houghton, MI, USA
| | - A S Barber
- Department of Physics and Astronomy, University of Utah, Salt Lake City, UT, USA
| | | | - A Becerril
- Instituto de Física, Universidad Nacional Autónoma de México, Mexico City, Mexico
| | - E Belmont-Moreno
- Instituto de Física, Universidad Nacional Autónoma de México, Mexico City, Mexico
| | - S Y BenZvi
- Department of Physics and Astronomy, University of Rochester, Rochester, NY, USA
| | - D Berley
- Department of Physics, University of Maryland, College Park, MD, USA
| | - A Bernal
- Instituto de Astronomía, Universidad Nacional Autónoma de México, Mexico City, Mexico
| | - J Braun
- Department of Physics, University of Wisconsin-Madison, Madison, WI, USA
| | - C Brisbois
- Department of Physics, Michigan Technological University, Houghton, MI, USA
| | | | - T Capistrán
- Instituto Nacional de Astrofísica, Óptica y Electrónica, Puebla, Mexico
| | - A Carramiñana
- Instituto Nacional de Astrofísica, Óptica y Electrónica, Puebla, Mexico
| | - S Casanova
- Institute of Nuclear Physics Polish Academy of Sciences, Krakow, Poland.,Max-Planck Institute for Nuclear Physics, Heidelberg, Germany
| | - M Castillo
- Universidad Michoacana de San Nicolás de Hidalgo, Morelia, Mexico
| | - U Cotti
- Universidad Michoacana de San Nicolás de Hidalgo, Morelia, Mexico
| | - J Cotzomi
- Facultad de Ciencias Físico Matemáticas, Benemérita Universidad Autónoma de Puebla, Puebla, Mexico
| | - S Coutiño de León
- Instituto Nacional de Astrofísica, Óptica y Electrónica, Puebla, Mexico
| | - C De León
- Facultad de Ciencias Físico Matemáticas, Benemérita Universidad Autónoma de Puebla, Puebla, Mexico
| | - E De la Fuente
- Departamento de Física, Centro Universitario de Ciencias Exactas e Ingenierías, Universidad de Guadalajara, Guadalajara, Mexico
| | - B L Dingus
- Los Alamos National Laboratory, Los Alamos, NM, USA
| | - M A DuVernois
- Department of Physics, University of Wisconsin-Madison, Madison, WI, USA
| | - J C Díaz-Vélez
- Departamento de Física, Centro Universitario de Ciencias Exactas e Ingenierías, Universidad de Guadalajara, Guadalajara, Mexico
| | - R W Ellsworth
- School of Physics, Astronomy, and Computational Sciences, George Mason University, Fairfax, VA, USA
| | - K Engel
- Department of Physics, University of Maryland, College Park, MD, USA
| | - O Enríquez-Rivera
- Instituto de Geofísica, Universidad Nacional Autónoma de México, Mexico City, Mexico
| | - D W Fiorino
- Department of Physics, University of Maryland, College Park, MD, USA
| | - N Fraija
- Instituto de Astronomía, Universidad Nacional Autónoma de México, Mexico City, Mexico
| | - J A García-González
- Instituto de Física, Universidad Nacional Autónoma de México, Mexico City, Mexico
| | - F Garfias
- Instituto de Astronomía, Universidad Nacional Autónoma de México, Mexico City, Mexico
| | - M Gerhardt
- Department of Physics, Michigan Technological University, Houghton, MI, USA
| | - A González Muñoz
- Instituto de Física, Universidad Nacional Autónoma de México, Mexico City, Mexico
| | - M M González
- Instituto de Astronomía, Universidad Nacional Autónoma de México, Mexico City, Mexico
| | - J A Goodman
- Department of Physics, University of Maryland, College Park, MD, USA
| | - Z Hampel-Arias
- Department of Physics, University of Wisconsin-Madison, Madison, WI, USA
| | - J P Harding
- Los Alamos National Laboratory, Los Alamos, NM, USA
| | - S Hernández
- Instituto de Física, Universidad Nacional Autónoma de México, Mexico City, Mexico
| | - A Hernández-Almada
- Instituto de Física, Universidad Nacional Autónoma de México, Mexico City, Mexico
| | - J Hinton
- Max-Planck Institute for Nuclear Physics, Heidelberg, Germany
| | - B Hona
- Department of Physics, Michigan Technological University, Houghton, MI, USA
| | - C M Hui
- Astrophysics Office, NASA Marshall Space Flight Center Huntsville, AL, USA
| | - P Hüntemeyer
- Department of Physics, Michigan Technological University, Houghton, MI, USA
| | - A Iriarte
- Instituto de Astronomía, Universidad Nacional Autónoma de México, Mexico City, Mexico
| | - A Jardin-Blicq
- Max-Planck Institute for Nuclear Physics, Heidelberg, Germany
| | - V Joshi
- Max-Planck Institute for Nuclear Physics, Heidelberg, Germany
| | - S Kaufmann
- Universidad Autónoma de Chiapas, Tuxtla Gutiérrez, Chiapas, Mexico
| | - D Kieda
- Department of Physics and Astronomy, University of Utah, Salt Lake City, UT, USA
| | - A Lara
- Instituto de Geofísica, Universidad Nacional Autónoma de México, Mexico City, Mexico
| | - R J Lauer
- Department of Physics and Astronomy, University of New Mexico, Albuquerque, NM, USA
| | - W H Lee
- Instituto de Astronomía, Universidad Nacional Autónoma de México, Mexico City, Mexico
| | - D Lennarz
- School of Physics and Center for Relativistic Astrophysics, Georgia Institute of Technology, Atlanta, GA, USA
| | - H León Vargas
- Instituto de Física, Universidad Nacional Autónoma de México, Mexico City, Mexico
| | - J T Linnemann
- Department of Physics and Astronomy, Michigan State University, East Lansing, MI, USA
| | - A L Longinotti
- Instituto Nacional de Astrofísica, Óptica y Electrónica, Puebla, Mexico
| | - G Luis Raya
- Universidad Politecnica de Pachuca, Pachuca, Hidalgo, Mexico
| | - R Luna-García
- Centro de Investigación en Computación, Instituto Politécnico Nacional, Mexico City, Mexico
| | - R López-Coto
- Max-Planck Institute for Nuclear Physics, Heidelberg, Germany.
| | - K Malone
- Department of Physics, Pennsylvania State University, University Park, PA, USA
| | - S S Marinelli
- Department of Physics and Astronomy, Michigan State University, East Lansing, MI, USA
| | - O Martinez
- Facultad de Ciencias Físico Matemáticas, Benemérita Universidad Autónoma de Puebla, Puebla, Mexico
| | | | - J Martínez-Castro
- Centro de Investigación en Computación, Instituto Politécnico Nacional, Mexico City, Mexico
| | - H Martínez-Huerta
- Physics Department, Centro de Investigacion y de Estudios Avanzados del IPN, Mexico City, Mexico
| | - J A Matthews
- Department of Physics and Astronomy, University of New Mexico, Albuquerque, NM, USA
| | | | - E Moreno
- Facultad de Ciencias Físico Matemáticas, Benemérita Universidad Autónoma de Puebla, Puebla, Mexico
| | - M Mostafá
- Department of Physics, Pennsylvania State University, University Park, PA, USA
| | - L Nellen
- Instituto de Ciencias Nucleares, Universidad Nacional Autónoma de México, Mexico City, Mexico
| | - M Newbold
- Department of Physics and Astronomy, University of Utah, Salt Lake City, UT, USA
| | - M U Nisa
- Department of Physics and Astronomy, University of Rochester, Rochester, NY, USA
| | | | - R Pelayo
- Centro de Investigación en Computación, Instituto Politécnico Nacional, Mexico City, Mexico
| | - J Pretz
- Department of Physics, Pennsylvania State University, University Park, PA, USA
| | - E G Pérez-Pérez
- Universidad Politecnica de Pachuca, Pachuca, Hidalgo, Mexico
| | - Z Ren
- Department of Physics and Astronomy, University of New Mexico, Albuquerque, NM, USA
| | - C D Rho
- Department of Physics and Astronomy, University of Rochester, Rochester, NY, USA
| | - C Rivière
- Department of Physics, University of Maryland, College Park, MD, USA
| | - D Rosa-González
- Instituto Nacional de Astrofísica, Óptica y Electrónica, Puebla, Mexico
| | - M Rosenberg
- Department of Physics, Pennsylvania State University, University Park, PA, USA
| | - E Ruiz-Velasco
- Instituto de Física, Universidad Nacional Autónoma de México, Mexico City, Mexico
| | - H Salazar
- Facultad de Ciencias Físico Matemáticas, Benemérita Universidad Autónoma de Puebla, Puebla, Mexico
| | - F Salesa Greus
- Institute of Nuclear Physics Polish Academy of Sciences, Krakow, Poland.
| | - A Sandoval
- Instituto de Física, Universidad Nacional Autónoma de México, Mexico City, Mexico
| | - M Schneider
- Santa Cruz Institute for Particle Physics, University of California, Santa Cruz, Santa Cruz, CA, USA
| | - H Schoorlemmer
- Max-Planck Institute for Nuclear Physics, Heidelberg, Germany
| | - G Sinnis
- Los Alamos National Laboratory, Los Alamos, NM, USA
| | - A J Smith
- Department of Physics, University of Maryland, College Park, MD, USA
| | - R W Springer
- Department of Physics and Astronomy, University of Utah, Salt Lake City, UT, USA
| | - P Surajbali
- Max-Planck Institute for Nuclear Physics, Heidelberg, Germany
| | - I Taboada
- School of Physics and Center for Relativistic Astrophysics, Georgia Institute of Technology, Atlanta, GA, USA
| | - O Tibolla
- Universidad Autónoma de Chiapas, Tuxtla Gutiérrez, Chiapas, Mexico
| | - K Tollefson
- Department of Physics and Astronomy, Michigan State University, East Lansing, MI, USA
| | - I Torres
- Instituto Nacional de Astrofísica, Óptica y Electrónica, Puebla, Mexico
| | - T N Ukwatta
- Los Alamos National Laboratory, Los Alamos, NM, USA
| | - G Vianello
- Hansen Experimental Physics Laboratory Stanford University, Stanford, CA, USA
| | - T Weisgarber
- Department of Physics, University of Wisconsin-Madison, Madison, WI, USA
| | - S Westerhoff
- Department of Physics, University of Wisconsin-Madison, Madison, WI, USA
| | - I G Wisher
- Department of Physics, University of Wisconsin-Madison, Madison, WI, USA
| | - J Wood
- Department of Physics, University of Wisconsin-Madison, Madison, WI, USA
| | - T Yapici
- Department of Physics and Astronomy, Michigan State University, East Lansing, MI, USA
| | - G Yodh
- Department of Physics and Astronomy, University of California, Irvine, Irvine, CA, USA
| | - P W Younk
- Los Alamos National Laboratory, Los Alamos, NM, USA
| | - A Zepeda
- Physics Department, Centro de Investigacion y de Estudios Avanzados del IPN, Mexico City, Mexico.,Universidad Autónoma de Chiapas, Tuxtla Gutiérrez, Chiapas, Mexico
| | - H Zhou
- Los Alamos National Laboratory, Los Alamos, NM, USA.
| | - F Guo
- Los Alamos National Laboratory, Los Alamos, NM, USA
| | - J Hahn
- Max-Planck Institute for Nuclear Physics, Heidelberg, Germany
| | - H Li
- Los Alamos National Laboratory, Los Alamos, NM, USA
| | - H Zhang
- Los Alamos National Laboratory, Los Alamos, NM, USA
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42
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Boschini MJ, Torre SD, Gervasi M, Grandi D, Jóhannesson G, Vacca GL, Masi N, Moskalenko IV, Pensotti S, Porter TA, Quadrani L, Rancoita PG, Rozza D, Tacconi M. HelMod in the Works: From Direct Observations to the Local Interstellar Spectrum of Cosmic-Ray Electrons. THE ASTROPHYSICAL JOURNAL 2018; 854:94. [PMID: 34646044 PMCID: PMC8506982 DOI: 10.3847/1538-4357/aaa75e] [Citation(s) in RCA: 5] [Impact Index Per Article: 0.8] [Reference Citation Analysis] [Abstract] [Key Words] [Grants] [Track Full Text] [Subscribe] [Scholar Register] [Indexed: 05/23/2023]
Abstract
The local interstellar spectrum (LIS) of cosmic-ray (CR) electrons for the energy range 1 MeV to 1 TeV is derived using the most recent experimental results combined with the state-of-the-art models for CR propagation in the Galaxy and in the heliosphere. 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 model-data comparison. The optimized HelMod parameters are then used to adjust GALPROP parameters to predict a refined LIS with the procedure repeated subject to a convergence criterion. The parameter optimization uses an extensive data set of proton spectra from 1997 to 2015. The proposed CR electron LIS accommodates both the low-energy interstellar spectra measured by Voyager 1 as well as the high-energy observations by PAMELA and AMS-02 that are made deep in the heliosphere; it also accounts for Ulysses counting rate features measured out of the ecliptic plane. The interstellar and heliospheric propagation parameters derived in this study agree well with our earlier results for CR protons, helium nuclei, and anti-protons propagation and LIS obtained in the same framework.
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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
| | - G Jóhannesson
- Science Institute, University of Iceland, Dunhaga 3, IS-107 Reykjavik, Iceland
- NORDITA, Roslagstullsbacken 23, SE-106 91 Stockholm, Sweden
| | | | | | - 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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43
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Direct detection of a break in the teraelectronvolt cosmic-ray spectrum of electrons and positrons. Nature 2017. [PMID: 29186110 DOI: 10.1038/nature24475.] [Citation(s) in RCA: 1] [Impact Index Per Article: 0.1] [Reference Citation Analysis] [Abstract] [Journal Information] [Subscribe] [Scholar Register] [Indexed: 11/09/2022]
Abstract
High-energy cosmic-ray electrons and positrons (CREs), which lose energy quickly during their propagation, provide a probe of Galactic high-energy processes and may enable the observation of phenomena such as dark-matter particle annihilation or decay. The CRE spectrum has been measured directly up to approximately 2 teraelectronvolts in previous balloon- or space-borne experiments, and indirectly up to approximately 5 teraelectronvolts using ground-based Cherenkov γ-ray telescope arrays. Evidence for a spectral break in the teraelectronvolt energy range has been provided by indirect measurements, although the results were qualified by sizeable systematic uncertainties. Here we report a direct measurement of CREs in the energy range 25 gigaelectronvolts to 4.6 teraelectronvolts by the Dark Matter Particle Explorer (DAMPE) with unprecedentedly high energy resolution and low background. The largest part of the spectrum can be well fitted by a 'smoothly broken power-law' model rather than a single power-law model. The direct detection of a spectral break at about 0.9 teraelectronvolts confirms the evidence found by previous indirect measurements, clarifies the behaviour of the CRE spectrum at energies above 1 teraelectronvolt and sheds light on the physical origin of the sub-teraelectronvolt CREs.
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44
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Direct detection of a break in the teraelectronvolt cosmic-ray spectrum of electrons and positrons. Nature 2017; 552:63-66. [DOI: 10.1038/nature24475] [Citation(s) in RCA: 287] [Impact Index Per Article: 41.0] [Reference Citation Analysis] [Track Full Text] [Journal Information] [Subscribe] [Scholar Register] [Received: 06/28/2017] [Accepted: 10/04/2017] [Indexed: 11/09/2022]
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45
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Adriani O, Akaike Y, Asano K, Asaoka Y, Bagliesi MG, Bigongiari G, Binns WR, Bonechi S, Bongi M, Brogi P, Buckley JH, Cannady N, Castellini G, Checchia C, Cherry ML, Collazuol G, Di Felice V, Ebisawa K, Fuke H, Guzik TG, Hams T, Hareyama M, Hasebe N, Hibino K, Ichimura M, Ioka K, Ishizaki W, Israel MH, Javaid A, Kasahara K, Kataoka J, Kataoka R, Katayose Y, Kato C, Kawanaka N, Kawakubo Y, Krawczynski HS, Krizmanic JF, Kuramata S, Lomtadze T, Maestro P, Marrocchesi PS, Messineo AM, Mitchell JW, Miyake S, Mizutani K, Moiseev AA, Mori K, Mori M, Mori N, Motz HM, Munakata K, Murakami H, Nakahira S, Nishimura J, de Nolfo GA, Okuno S, Ormes JF, Ozawa S, Pacini L, Palma F, Papini P, Penacchioni AV, Rauch BF, Ricciarini SB, Sakai K, Sakamoto T, Sasaki M, Shimizu Y, Shiomi A, Sparvoli R, Spillantini P, Stolzi F, Takahashi I, Takayanagi M, Takita M, Tamura T, Tateyama N, Terasawa T, Tomida H, Torii S, Tsunesada Y, Uchihori Y, Ueno S, Vannuccini E, Wefel JP, Yamaoka K, Yanagita S, Yoshida A, Yoshida K, Yuda T. Energy Spectrum of Cosmic-Ray Electron and Positron from 10 GeV to 3 TeV Observed with the Calorimetric Electron Telescope on the International Space Station. PHYSICAL REVIEW LETTERS 2017; 119:181101. [PMID: 29219544 DOI: 10.1103/physrevlett.119.181101] [Citation(s) in RCA: 32] [Impact Index Per Article: 4.6] [Reference Citation Analysis] [Abstract] [Track Full Text] [Subscribe] [Scholar Register] [Received: 08/09/2017] [Indexed: 06/07/2023]
Abstract
First results of a cosmic-ray electron and positron spectrum from 10 GeV to 3 TeV is presented based upon observations with the CALET instrument on the International Space Station starting in October, 2015. Nearly a half million electron and positron events are included in the analysis. CALET is an all-calorimetric instrument with total vertical thickness of 30 X_{0} and a fine imaging capability designed to achieve a large proton rejection and excellent energy resolution well into the TeV energy region. The observed energy spectrum over 30 GeV can be fit with a single power law with a spectral index of -3.152±0.016 (stat+syst). Possible structure observed above 100 GeV requires further investigation with increased statistics and refined data analysis.
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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
- of Physics, University of Maryland, Baltimore County, 1000 Hilltop Circle, Baltimore, Maryland 21250, USA
- Astroparticle Physics Laboratory, NASA/GSFC, Greenbelt, Maryland 20771, USA
| | - K Asano
- Institute for Cosmic Ray Research, The University of Tokyo, 5-1-5 Kashiwa-no-Ha, Kashiwa, Chiba 277-8582, Japan
| | - Y Asaoka
- Research Institute for Science and Engineering, Waseda University, 3-4-1 Okubo, Shinjuku, Tokyo 169-8555, Japan
- JEM Utilization Center, Human Spaceflight Technology Directorate, Japan Aerospace Exploration Agency, 2-1-1 Sengen, Tsukuba, Ibaraki 305-8505, Japan
| | - M G Bagliesi
- 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
| | - 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, Washington University, One Brookings Drive, St. Louis, Missouri 63130-4899, USA
| | - S Bonechi
- 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 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
| | - J H Buckley
- Department of Physics, Washington University, One Brookings Drive, St. Louis, Missouri 63130-4899, USA
| | - N Cannady
- Department of Physics and Astronomy, Louisiana State University, 202 Nicholson Hall, Baton Rouge, Louisiana 70803, 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 Physics and Astronomy, University of Padova, Via Marzolo, 8, 35131 Padova, Italy
- INFN Sezione di Padova, Via Marzolo, 8, 35131 Padova, 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
| | - V Di Felice
- University of Rome "Tor Vergata," Via della Ricerca Scientifica 1, 00133 Rome, Italy
- INFN Sezione di Rome "Tor Vergata," Via della Ricerca Scientifica 1, 00133 Rome, Italy
| | - K Ebisawa
- Institute of Space and Astronautical Science, Japan Aerospace Exploration Agency, 3-1-1 Yoshinodai, Chuo, Sagamihara, Kanagawa 252-5210, Japan
| | - H Fuke
- Institute of Space and Astronautical Science, Japan Aerospace Exploration Agency, 3-1-1 Yoshinodai, Chuo, Sagamihara, Kanagawa 252-5210, Japan
| | - T G Guzik
- Department of Physics and Astronomy, Louisiana State University, 202 Nicholson Hall, Baton Rouge, Louisiana 70803, USA
| | - T Hams
- of Physics, University of Maryland, Baltimore County, 1000 Hilltop Circle, Baltimore, Maryland 21250, USA
- CRESST and Astroparticle Physics Laboratory NASA/GSFC, Greenbelt, Maryland 20771, USA
| | - M Hareyama
- St. Marianna University School of Medicine, 2-16-1, Sugao, Miyamae-ku, Kawasaki, Kanagawa 216-8511, Japan
| | - N Hasebe
- Research Institute for Science and Engineering, Waseda University, 3-4-1 Okubo, Shinjuku, Tokyo 169-8555, Japan
| | - 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 Oiwakecho, Sakyo, 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, Washington University, One Brookings Drive, St. Louis, Missouri 63130-4899, USA
| | - A Javaid
- Department of Physics and Astronomy, Louisiana State University, 202 Nicholson Hall, Baton Rouge, Louisiana 70803, USA
| | - K Kasahara
- Research Institute for Science and Engineering, Waseda University, 3-4-1 Okubo, Shinjuku, Tokyo 169-8555, Japan
| | - J Kataoka
- Research Institute for 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
- Hakubi Center, Kyoto University, Yoshida Honmachi, Sakyo-ku, Kyoto 606-8501, Japan
- Department of Astronomy, Graduate School of Science, Kyoto University, Kitashirakawa Oiwake-cho, Sakyo-ku, Kyoto 606-8502, Japan
| | - Y Kawakubo
- College of Science and Engineering, Department of Physics and Mathematics, Aoyama Gakuin University, 5-10-1 Fuchinobe, Chuo, Sagamihara, Kanagawa 252-5258, Japan
| | - H S Krawczynski
- Department of Physics, Washington University, One Brookings Drive, St. Louis, Missouri 63130-4899, USA
| | - J F Krizmanic
- of Physics, University of Maryland, Baltimore County, 1000 Hilltop Circle, Baltimore, Maryland 21250, USA
- CRESST and Astroparticle Physics Laboratory NASA/GSFC, Greenbelt, Maryland 20771, USA
| | - S Kuramata
- Faculty of Science and Technology, Graduate School of Science and Technology, Hirosaki University, 3, Bunkyo, Hirosaki, Aomori 036-8561, Japan
| | - T Lomtadze
- 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
| | - 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
| | - K Mizutani
- Saitama University, Shimo-Okubo 255, Sakura, Saitama 338-8570, Japan
| | - A A Moiseev
- CRESST and Astroparticle Physics Laboratory NASA/GSFC, Greenbelt, Maryland 20771, USA
- Department of Astronomy, University of Maryland, College Park, Maryland 20742, USA
| | - K Mori
- Research Institute for Science and Engineering, Waseda University, 3-4-1 Okubo, Shinjuku, Tokyo 169-8555, Japan
- Institute of Space and Astronautical Science, Japan Aerospace Exploration Agency, 3-1-1 Yoshinodai, Chuo, Sagamihara, Kanagawa 252-5210, Japan
| | - 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
- International Center for Science and Engineering Programs, 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
| | - H Murakami
- Research Institute for Science and Engineering, Waseda University, 3-4-1 Okubo, Shinjuku, Tokyo 169-8555, Japan
| | - S Nakahira
- RIKEN, 2-1 Hirosawa, Wako, Saitama 351-0198, 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
| | - S Ozawa
- Research Institute for Science and Engineering, Waseda University, 3-4-1 Okubo, Shinjuku, Tokyo 169-8555, 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
| | - F Palma
- University of Rome "Tor Vergata," Via della Ricerca Scientifica 1, 00133 Rome, Italy
- INFN Sezione di Rome "Tor Vergata," Via della Ricerca Scientifica 1, 00133 Rome, Italy
| | - P Papini
- INFN Sezione di Florence, Via Sansone, 1-50019 Sesto, Fiorentino, Italy
| | - A V Penacchioni
- Department of Physical Sciences, Earth and Environment, University of Siena, via Roma 56, 53100 Siena, Italy
- ASI Science Data Center (ASDC), Via del Politecnico snc, 00133 Rome, Italy
| | - B F Rauch
- Department of Physics, 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
- of Physics, University of Maryland, Baltimore County, 1000 Hilltop Circle, Baltimore, Maryland 21250, USA
- CRESST and Astroparticle Physics Laboratory 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
- CRESST and Astroparticle Physics Laboratory 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
| | - R Sparvoli
- University of Rome "Tor Vergata," Via della Ricerca Scientifica 1, 00133 Rome, Italy
- INFN Sezione di Rome "Tor Vergata," Via della Ricerca Scientifica 1, 00133 Rome, Italy
| | - 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
| | - I Takahashi
- Kavli Institute for the Physics and Mathematics of the Universe, The University of Tokyo, 5-1-5 Kashiwanoha, Kashiwa 277-8583, Japan
| | - M Takayanagi
- Institute of Space and Astronautical Science, Japan Aerospace Exploration Agency, 3-1-1 Yoshinodai, Chuo, Sagamihara, Kanagawa 252-5210, Japan
| | - 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
| | - N Tateyama
- Kanagawa University, 3-27-1 Rokkakubashi, Kanagawa, Yokohama, Kanagawa 221-8686, Japan
| | - T Terasawa
- RIKEN, 2-1 Hirosawa, Wako, Saitama 351-0198, Japan
| | - H Tomida
- Institute of Space and Astronautical Science, Japan Aerospace Exploration Agency, 3-1-1 Yoshinodai, Chuo, Sagamihara, Kanagawa 252-5210, Japan
| | - S Torii
- Research Institute for Science and Engineering, Waseda University, 3-4-1 Okubo, Shinjuku, Tokyo 169-8555, Japan
- JEM Utilization Center, Human Spaceflight Technology Directorate, Japan Aerospace Exploration Agency, 2-1-1 Sengen, Tsukuba, Ibaraki 305-8505, Japan
- School of Advanced Science and Engineering, Waseda University, 3-4-1 Okubo, Shinjuku, Tokyo 169-8555, Japan
| | - Y Tsunesada
- Division of Mathematics and Physics, Graduate School of Science, 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
| | - S Ueno
- Institute of Space and Astronautical Science, Japan Aerospace Exploration Agency, 3-1-1 Yoshinodai, Chuo, Sagamihara, Kanagawa 252-5210, 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
| | - T Yuda
- Institute for Cosmic Ray Research, The University of Tokyo, 5-1-5 Kashiwa-no-Ha, Kashiwa, Chiba 277-8582, Japan
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Lees JP, Poireau V, Tisserand V, Grauges E, Palano A, Eigen G, Brown DN, Derdzinski M, Giuffrida A, Kolomensky YG, Fritsch M, Koch H, Schroeder T, Hearty C, Mattison TS, McKenna JA, So RY, Blinov VE, Buzykaev AR, Druzhinin VP, Golubev VB, Kravchenko EA, Onuchin AP, Serednyakov SI, Skovpen YI, Solodov EP, Todyshev KY, Lankford AJ, Gary JW, Long O, Eisner AM, Lockman WS, Panduro Vazquez W, Chao DS, Cheng CH, Echenard B, Flood KT, Hitlin DG, Kim J, Miyashita TS, Ongmongkolkul P, Porter FC, Röhrken M, Huard Z, Meadows BT, Pushpawela BG, Sokoloff MD, Sun L, Smith JG, Wagner SR, Bernard D, Verderi M, Bettoni D, Bozzi C, Calabrese R, Cibinetto G, Fioravanti E, Garzia I, Luppi E, Santoro V, Calcaterra A, de Sangro R, Finocchiaro G, Martellotti S, Patteri P, Peruzzi IM, Piccolo M, Rotondo M, Zallo A, Passaggio S, Patrignani C, Lacker HM, Bhuyan B, Mallik U, Chen C, Cochran J, Prell S, Ahmed H, Gritsan AV, Arnaud N, Davier M, Le Diberder F, Lutz AM, Wormser G, Lange DJ, Wright DM, Coleman JP, Gabathuler E, Hutchcroft DE, Payne DJ, Touramanis C, Bevan AJ, Di Lodovico F, Sacco R, Cowan G, Banerjee S, Brown DN, Davis CL, Denig AG, Gradl W, Griessinger K, Hafner A, Schubert KR, Barlow RJ, Lafferty GD, Cenci R, Jawahery A, Roberts DA, Cowan R, Robertson SH, Dey B, Neri N, Palombo F, Cheaib R, Cremaldi L, Godang R, Summers DJ, Taras P, De Nardo G, Sciacca C, Raven G, Jessop CP, LoSecco JM, Honscheid K, Kass R, Gaz A, Margoni M, Posocco M, Simi G, Simonetto F, Stroili R, Akar S, Ben-Haim E, Bomben M, Bonneaud GR, Calderini G, Chauveau J, Marchiori G, Ocariz J, Biasini M, Manoni E, Rossi A, Batignani G, Bettarini S, Carpinelli M, Casarosa G, Chrzaszcz M, Forti F, Giorgi MA, Lusiani A, Oberhof B, Paoloni E, Rama M, Rizzo G, Walsh JJ, Smith AJS, Anulli F, Faccini R, Ferrarotto F, Ferroni F, Pilloni A, Piredda G, Bünger C, Dittrich S, Grünberg O, Heß M, Leddig T, Voß C, Waldi R, Adye T, Wilson FF, Emery S, Vasseur G, Aston D, Cartaro C, Convery MR, Dorfan J, Dunwoodie W, Ebert M, Field RC, Fulsom BG, Graham MT, Hast C, Innes WR, Kim P, Leith DWGS, Luitz S, MacFarlane DB, Muller DR, Neal H, Ratcliff BN, Roodman A, Sullivan MK, Va'vra J, Wisniewski WJ, Purohit MV, Wilson JR, Randle-Conde A, Sekula SJ, Bellis M, Burchat PR, Puccio EMT, Alam MS, Ernst JA, Gorodeisky R, Guttman N, Peimer DR, Soffer A, Spanier SM, Ritchie JL, Schwitters RF, Izen JM, Lou XC, Bianchi F, De Mori F, Filippi A, Gamba D, Lanceri L, Vitale L, Martinez-Vidal F, Oyanguren A, Albert J, Beaulieu A, Bernlochner FU, King GJ, Kowalewski R, Lueck T, Nugent IM, Roney JM, Sobie RJ, Tasneem N, Gershon TJ, Harrison PF, Latham TE, Prepost R, Wu SL. Search for Invisible Decays of a Dark Photon Produced in e^{+}e^{-} Collisions at BaBar. PHYSICAL REVIEW LETTERS 2017; 119:131804. [PMID: 29341718 DOI: 10.1103/physrevlett.119.131804] [Citation(s) in RCA: 12] [Impact Index Per Article: 1.7] [Reference Citation Analysis] [Abstract] [Track Full Text] [Subscribe] [Scholar Register] [Received: 02/14/2017] [Indexed: 06/07/2023]
Abstract
We search for single-photon events in 53 fb^{-1} of e^{+}e^{-} collision data collected with the BABAR detector at the PEP-II B-Factory. We look for events with a single high-energy photon and a large missing momentum and energy, consistent with production of a spin-1 particle A^{'} through the process e^{+}e^{-}→γA^{'}; A^{'}→invisible. Such particles, referred to as "dark photons," are motivated by theories applying a U(1) gauge symmetry to dark matter. We find no evidence for such processes and set 90% confidence level upper limits on the coupling strength of A^{'} to e^{+}e^{-} in the mass range m_{A^{'}}≤8 GeV. In particular, our limits exclude the values of the A^{'} coupling suggested by the dark-photon interpretation of the muon (g-2)_{μ} anomaly, as well as a broad range of parameters for the dark-sector models.
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Affiliation(s)
- J P Lees
- Laboratoire d'Annecy-le-Vieux de Physique des Particules (LAPP), Université de Savoie, CNRS/IN2P3, F-74941 Annecy-Le-Vieux, France
| | - V Poireau
- Laboratoire d'Annecy-le-Vieux de Physique des Particules (LAPP), Université de Savoie, CNRS/IN2P3, F-74941 Annecy-Le-Vieux, France
| | - V Tisserand
- Laboratoire d'Annecy-le-Vieux de Physique des Particules (LAPP), Université de Savoie, CNRS/IN2P3, F-74941 Annecy-Le-Vieux, France
| | - E Grauges
- Universitat de Barcelona, Facultat de Fisica, Departament ECM, E-08028 Barcelona, Spain
| | - A Palano
- INFN Sezione di Bari and Dipartimento di Fisica, Università di Bari, I-70126 Bari, Italy
| | - G Eigen
- University of Bergen, Institute of Physics, N-5007 Bergen, Norway
| | - D N Brown
- Lawrence Berkeley National Laboratory and University of California, Berkeley, California 94720, USA
| | - M Derdzinski
- Lawrence Berkeley National Laboratory and University of California, Berkeley, California 94720, USA
| | - A Giuffrida
- Lawrence Berkeley National Laboratory and University of California, Berkeley, California 94720, USA
| | - Yu G Kolomensky
- Lawrence Berkeley National Laboratory and University of California, Berkeley, California 94720, USA
| | - M Fritsch
- Ruhr Universität Bochum, Institut für Experimentalphysik 1, D-44780 Bochum, Germany
| | - H Koch
- Ruhr Universität Bochum, Institut für Experimentalphysik 1, D-44780 Bochum, Germany
| | - T Schroeder
- Ruhr Universität Bochum, Institut für Experimentalphysik 1, D-44780 Bochum, Germany
| | - C Hearty
- Institute of Particle Physics, Vancouver, British Columbia V6T 1Z1, Canada
- University of British Columbia, Vancouver, British Columbia V6T 1Z1, Canada
| | - T S Mattison
- University of British Columbia, Vancouver, British Columbia V6T 1Z1, Canada
| | - J A McKenna
- University of British Columbia, Vancouver, British Columbia V6T 1Z1, Canada
| | - R Y So
- University of British Columbia, Vancouver, British Columbia V6T 1Z1, Canada
| | - V E Blinov
- Budker Institute of Nuclear Physics SB RAS, Novosibirsk 630090, Russia
- Novosibirsk State University, Novosibirsk 630090, Russia
- Novosibirsk State Technical University, Novosibirsk 630092, Russia
| | - A R Buzykaev
- Budker Institute of Nuclear Physics SB RAS, Novosibirsk 630090, Russia
| | - V P Druzhinin
- Budker Institute of Nuclear Physics SB RAS, Novosibirsk 630090, Russia
- Novosibirsk State University, Novosibirsk 630090, Russia
| | - V B Golubev
- Budker Institute of Nuclear Physics SB RAS, Novosibirsk 630090, Russia
- Novosibirsk State University, Novosibirsk 630090, Russia
| | - E A Kravchenko
- Budker Institute of Nuclear Physics SB RAS, Novosibirsk 630090, Russia
- Novosibirsk State University, Novosibirsk 630090, Russia
| | - A P Onuchin
- Budker Institute of Nuclear Physics SB RAS, Novosibirsk 630090, Russia
- Novosibirsk State University, Novosibirsk 630090, Russia
- Novosibirsk State Technical University, Novosibirsk 630092, Russia
| | - S I Serednyakov
- Budker Institute of Nuclear Physics SB RAS, Novosibirsk 630090, Russia
- Novosibirsk State University, Novosibirsk 630090, Russia
| | - Yu I Skovpen
- Budker Institute of Nuclear Physics SB RAS, Novosibirsk 630090, Russia
- Novosibirsk State University, Novosibirsk 630090, Russia
| | - E P Solodov
- Budker Institute of Nuclear Physics SB RAS, Novosibirsk 630090, Russia
- Novosibirsk State University, Novosibirsk 630090, Russia
| | - K Yu Todyshev
- Budker Institute of Nuclear Physics SB RAS, Novosibirsk 630090, Russia
- Novosibirsk State University, Novosibirsk 630090, Russia
| | - A J Lankford
- University of California at Irvine, Irvine, California 92697, USA
| | - J W Gary
- University of California at Riverside, Riverside, California 92521, USA
| | - O Long
- University of California at Riverside, Riverside, California 92521, USA
| | - A M Eisner
- University of California at Santa Cruz, Institute for Particle Physics, Santa Cruz, California 95064, USA
| | - W S Lockman
- University of California at Santa Cruz, Institute for Particle Physics, Santa Cruz, California 95064, USA
| | - W Panduro Vazquez
- University of California at Santa Cruz, Institute for Particle Physics, Santa Cruz, California 95064, USA
| | - D S Chao
- California Institute of Technology, Pasadena, California 91125, USA
| | - C H Cheng
- California Institute of Technology, Pasadena, California 91125, USA
| | - B Echenard
- California Institute of Technology, Pasadena, California 91125, USA
| | - K T Flood
- California Institute of Technology, Pasadena, California 91125, USA
| | - D G Hitlin
- California Institute of Technology, Pasadena, California 91125, USA
| | - J Kim
- California Institute of Technology, Pasadena, California 91125, USA
| | - T S Miyashita
- California Institute of Technology, Pasadena, California 91125, USA
| | - P Ongmongkolkul
- California Institute of Technology, Pasadena, California 91125, USA
| | - F C Porter
- California Institute of Technology, Pasadena, California 91125, USA
| | - M Röhrken
- California Institute of Technology, Pasadena, California 91125, USA
| | - Z Huard
- University of Cincinnati, Cincinnati, Ohio 45221, USA
| | - B T Meadows
- University of Cincinnati, Cincinnati, Ohio 45221, USA
| | | | - M D Sokoloff
- University of Cincinnati, Cincinnati, Ohio 45221, USA
| | - L Sun
- University of Cincinnati, Cincinnati, Ohio 45221, USA
| | - J G Smith
- University of Colorado, Boulder, Colorado 80309, USA
| | - S R Wagner
- University of Colorado, Boulder, Colorado 80309, USA
| | - D Bernard
- Laboratoire Leprince-Ringuet, Ecole Polytechnique, CNRS/IN2P3, F-91128 Palaiseau, France
| | - M Verderi
- Laboratoire Leprince-Ringuet, Ecole Polytechnique, CNRS/IN2P3, F-91128 Palaiseau, France
| | - D Bettoni
- INFN Sezione di Ferrara, I-44122 Ferrara, Italy
| | - C Bozzi
- INFN Sezione di Ferrara, I-44122 Ferrara, Italy
| | - R Calabrese
- INFN Sezione di Ferrara, I-44122 Ferrara, Italy
- Dipartimento di Fisica e Scienze della Terra, Università di Ferrara, I-44122 Ferrara, Italy
| | - G Cibinetto
- INFN Sezione di Ferrara, I-44122 Ferrara, Italy
- Dipartimento di Fisica e Scienze della Terra, Università di Ferrara, I-44122 Ferrara, Italy
| | - E Fioravanti
- INFN Sezione di Ferrara, I-44122 Ferrara, Italy
- Dipartimento di Fisica e Scienze della Terra, Università di Ferrara, I-44122 Ferrara, Italy
| | - I Garzia
- INFN Sezione di Ferrara, I-44122 Ferrara, Italy
- Dipartimento di Fisica e Scienze della Terra, Università di Ferrara, I-44122 Ferrara, Italy
| | - E Luppi
- INFN Sezione di Ferrara, I-44122 Ferrara, Italy
- Dipartimento di Fisica e Scienze della Terra, Università di Ferrara, I-44122 Ferrara, Italy
| | - V Santoro
- INFN Sezione di Ferrara, I-44122 Ferrara, Italy
| | - A Calcaterra
- INFN Laboratori Nazionali di Frascati, I-00044 Frascati, Italy
| | - R de Sangro
- INFN Laboratori Nazionali di Frascati, I-00044 Frascati, Italy
| | - G Finocchiaro
- INFN Laboratori Nazionali di Frascati, I-00044 Frascati, Italy
| | - S Martellotti
- INFN Laboratori Nazionali di Frascati, I-00044 Frascati, Italy
| | - P Patteri
- INFN Laboratori Nazionali di Frascati, I-00044 Frascati, Italy
| | - I M Peruzzi
- INFN Laboratori Nazionali di Frascati, I-00044 Frascati, Italy
| | - M Piccolo
- INFN Laboratori Nazionali di Frascati, I-00044 Frascati, Italy
| | - M Rotondo
- INFN Laboratori Nazionali di Frascati, I-00044 Frascati, Italy
| | - A Zallo
- INFN Laboratori Nazionali di Frascati, I-00044 Frascati, Italy
| | - S Passaggio
- INFN Sezione di Genova, I-16146 Genova, Italy
| | | | - H M Lacker
- Humboldt-Universität zu Berlin, Institut für Physik, D-12489 Berlin, Germany
| | - B Bhuyan
- Indian Institute of Technology Guwahati, Guwahati, Assam 781 039, India
| | - U Mallik
- University of Iowa, Iowa City, Iowa 52242, USA
| | - C Chen
- Iowa State University, Ames, Iowa 50011, USA
| | - J Cochran
- Iowa State University, Ames, Iowa 50011, USA
| | - S Prell
- Iowa State University, Ames, Iowa 50011, USA
| | - H Ahmed
- Physics Department, Jazan University, Jazan 22822, Saudi Arabia
| | - A V Gritsan
- Johns Hopkins University, Baltimore, Maryland 21218, USA
| | - N Arnaud
- Laboratoire de l'Accélérateur Linéaire, IN2P3/CNRS et Université Paris-Sud 11, Centre Scientifique d'Orsay, F-91898 Orsay Cedex, France
| | - M Davier
- Laboratoire de l'Accélérateur Linéaire, IN2P3/CNRS et Université Paris-Sud 11, Centre Scientifique d'Orsay, F-91898 Orsay Cedex, France
| | - F Le Diberder
- Laboratoire de l'Accélérateur Linéaire, IN2P3/CNRS et Université Paris-Sud 11, Centre Scientifique d'Orsay, F-91898 Orsay Cedex, France
| | - A M Lutz
- Laboratoire de l'Accélérateur Linéaire, IN2P3/CNRS et Université Paris-Sud 11, Centre Scientifique d'Orsay, F-91898 Orsay Cedex, France
| | - G Wormser
- Laboratoire de l'Accélérateur Linéaire, IN2P3/CNRS et Université Paris-Sud 11, Centre Scientifique d'Orsay, F-91898 Orsay Cedex, France
| | - D J Lange
- Lawrence Livermore National Laboratory, Livermore, California 94550, USA
| | - D M Wright
- Lawrence Livermore National Laboratory, Livermore, California 94550, USA
| | - J P Coleman
- University of Liverpool, Liverpool L69 7ZE, United Kingdom
| | - E Gabathuler
- University of Liverpool, Liverpool L69 7ZE, United Kingdom
| | - D E Hutchcroft
- University of Liverpool, Liverpool L69 7ZE, United Kingdom
| | - D J Payne
- University of Liverpool, Liverpool L69 7ZE, United Kingdom
| | - C Touramanis
- University of Liverpool, Liverpool L69 7ZE, United Kingdom
| | - A J Bevan
- Queen Mary, University of London, London E1 4NS, United Kingdom
| | - F Di Lodovico
- Queen Mary, University of London, London E1 4NS, United Kingdom
| | - R Sacco
- Queen Mary, University of London, London E1 4NS, United Kingdom
| | - G Cowan
- University of London, Royal Holloway and Bedford New College, Egham, Surrey TW20 0EX, United Kingdom
| | - Sw Banerjee
- University of Louisville, Louisville, Kentucky 40292, USA
| | - D N Brown
- University of Louisville, Louisville, Kentucky 40292, USA
| | - C L Davis
- University of Louisville, Louisville, Kentucky 40292, USA
| | - A G Denig
- Johannes Gutenberg-Universität Mainz, Institut für Kernphysik, D-55099 Mainz, Germany
| | - W Gradl
- Johannes Gutenberg-Universität Mainz, Institut für Kernphysik, D-55099 Mainz, Germany
| | - K Griessinger
- Johannes Gutenberg-Universität Mainz, Institut für Kernphysik, D-55099 Mainz, Germany
| | - A Hafner
- Johannes Gutenberg-Universität Mainz, Institut für Kernphysik, D-55099 Mainz, Germany
| | - K R Schubert
- Johannes Gutenberg-Universität Mainz, Institut für Kernphysik, D-55099 Mainz, Germany
| | - R J Barlow
- University of Manchester, Manchester M13 9PL, United Kingdom
| | - G D Lafferty
- University of Manchester, Manchester M13 9PL, United Kingdom
| | - R Cenci
- University of Maryland, College Park, Maryland 20742, USA
| | - A Jawahery
- University of Maryland, College Park, Maryland 20742, USA
| | - D A Roberts
- University of Maryland, College Park, Maryland 20742, USA
| | - R Cowan
- Massachusetts Institute of Technology, Laboratory for Nuclear Science, Cambridge, Massachusetts 02139, USA
| | - S H Robertson
- Institute of Particle Physics and McGill University, Montréal, Québec H3A 2T8, Canada
| | - B Dey
- INFN Sezione di Milano, I-20133 Milano, Italy
| | - N Neri
- INFN Sezione di Milano, I-20133 Milano, Italy
| | - F Palombo
- INFN Sezione di Milano, I-20133 Milano, Italy
- Dipartimento di Fisica, Università di Milano, I-20133 Milano, Italy
| | - R Cheaib
- University of Mississippi, University, Mississippi 38677, USA
| | - L Cremaldi
- University of Mississippi, University, Mississippi 38677, USA
| | - R Godang
- University of Mississippi, University, Mississippi 38677, USA
| | - D J Summers
- University of Mississippi, University, Mississippi 38677, USA
| | - P Taras
- Université de Montréal, Physique des Particules, Montréal, Québec H3C 3J7, Canada
| | - G De Nardo
- INFN Sezione di Napoli and Dipartimento di Scienze Fisiche, Università di Napoli Federico II, I-80126 Napoli, Italy
| | - C Sciacca
- INFN Sezione di Napoli and Dipartimento di Scienze Fisiche, Università di Napoli Federico II, I-80126 Napoli, Italy
| | - G Raven
- NIKHEF, National Institute for Nuclear Physics and High Energy Physics, NL-1009 DB Amsterdam, Netherlands
| | - C P Jessop
- University of Notre Dame, Notre Dame, Indiana 46556, USA
| | - J M LoSecco
- University of Notre Dame, Notre Dame, Indiana 46556, USA
| | - K Honscheid
- The Ohio State University, Columbus, Ohio 43210, USA
| | - R Kass
- The Ohio State University, Columbus, Ohio 43210, USA
| | - A Gaz
- INFN Sezione di Padova, I-35131 Padova, Italy
| | - M Margoni
- INFN Sezione di Padova, I-35131 Padova, Italy
- Dipartimento di Fisica, Università di Padova, I-35131 Padova, Italy
| | - M Posocco
- INFN Sezione di Padova, I-35131 Padova, Italy
| | - G Simi
- INFN Sezione di Padova, I-35131 Padova, Italy
- Dipartimento di Fisica, Università di Padova, I-35131 Padova, Italy
| | - F Simonetto
- INFN Sezione di Padova, I-35131 Padova, Italy
- Dipartimento di Fisica, Università di Padova, I-35131 Padova, Italy
| | - R Stroili
- INFN Sezione di Padova, I-35131 Padova, Italy
- Dipartimento di Fisica, Università di Padova, I-35131 Padova, Italy
| | - S Akar
- Laboratoire de Physique Nucléaire et de Hautes Energies, IN2P3/CNRS, Université Pierre et Marie Curie-Paris 6, Université Denis Diderot-Paris 7, F-75252 Paris, France
| | - E Ben-Haim
- Laboratoire de Physique Nucléaire et de Hautes Energies, IN2P3/CNRS, Université Pierre et Marie Curie-Paris 6, Université Denis Diderot-Paris 7, F-75252 Paris, France
| | - M Bomben
- Laboratoire de Physique Nucléaire et de Hautes Energies, IN2P3/CNRS, Université Pierre et Marie Curie-Paris 6, Université Denis Diderot-Paris 7, F-75252 Paris, France
| | - G R Bonneaud
- Laboratoire de Physique Nucléaire et de Hautes Energies, IN2P3/CNRS, Université Pierre et Marie Curie-Paris 6, Université Denis Diderot-Paris 7, F-75252 Paris, France
| | - G Calderini
- Laboratoire de Physique Nucléaire et de Hautes Energies, IN2P3/CNRS, Université Pierre et Marie Curie-Paris 6, Université Denis Diderot-Paris 7, F-75252 Paris, France
| | - J Chauveau
- Laboratoire de Physique Nucléaire et de Hautes Energies, IN2P3/CNRS, Université Pierre et Marie Curie-Paris 6, Université Denis Diderot-Paris 7, F-75252 Paris, France
| | - G Marchiori
- Laboratoire de Physique Nucléaire et de Hautes Energies, IN2P3/CNRS, Université Pierre et Marie Curie-Paris 6, Université Denis Diderot-Paris 7, F-75252 Paris, France
| | - J Ocariz
- Laboratoire de Physique Nucléaire et de Hautes Energies, IN2P3/CNRS, Université Pierre et Marie Curie-Paris 6, Université Denis Diderot-Paris 7, F-75252 Paris, France
| | - M Biasini
- INFN Sezione di Perugia, I-06123 Perugia, Italy
- Dipartimento di Fisica, Università di Perugia, I-06123 Perugia, Italy
| | - E Manoni
- INFN Sezione di Perugia, I-06123 Perugia, Italy
| | - A Rossi
- INFN Sezione di Perugia, I-06123 Perugia, Italy
| | - G Batignani
- INFN Sezione di Pisa, I-56127 Pisa, Italy
- Dipartimento di Fisica, Università di Pisa, I-56127 Pisa, Italy
| | - S Bettarini
- INFN Sezione di Pisa, I-56127 Pisa, Italy
- Dipartimento di Fisica, Università di Pisa, I-56127 Pisa, Italy
| | - M Carpinelli
- INFN Sezione di Pisa, I-56127 Pisa, Italy
- Dipartimento di Fisica, Università di Pisa, I-56127 Pisa, Italy
| | - G Casarosa
- INFN Sezione di Pisa, I-56127 Pisa, Italy
- Dipartimento di Fisica, Università di Pisa, I-56127 Pisa, Italy
| | | | - F Forti
- INFN Sezione di Pisa, I-56127 Pisa, Italy
- Dipartimento di Fisica, Università di Pisa, I-56127 Pisa, Italy
| | - M A Giorgi
- INFN Sezione di Pisa, I-56127 Pisa, Italy
- Dipartimento di Fisica, Università di Pisa, I-56127 Pisa, Italy
| | - A Lusiani
- INFN Sezione di Pisa, I-56127 Pisa, Italy
- Scuola Normale Superiore di Pisa, I-56127 Pisa, Italy
| | - B Oberhof
- INFN Sezione di Pisa, I-56127 Pisa, Italy
- Dipartimento di Fisica, Università di Pisa, I-56127 Pisa, Italy
| | - E Paoloni
- INFN Sezione di Pisa, I-56127 Pisa, Italy
- Dipartimento di Fisica, Università di Pisa, I-56127 Pisa, Italy
| | - M Rama
- INFN Sezione di Pisa, I-56127 Pisa, Italy
| | - G Rizzo
- INFN Sezione di Pisa, I-56127 Pisa, Italy
- Dipartimento di Fisica, Università di Pisa, I-56127 Pisa, Italy
| | - J J Walsh
- INFN Sezione di Pisa, I-56127 Pisa, Italy
| | - A J S Smith
- Princeton University, Princeton, New Jersey 08544, USA
| | - F Anulli
- INFN Sezione di Roma, I-00185 Roma, Italy
| | - R Faccini
- INFN Sezione di Roma, I-00185 Roma, Italy
- Dipartimento di Fisica, Università di Roma La Sapienza, I-00185 Roma, Italy
| | | | - F Ferroni
- INFN Sezione di Roma, I-00185 Roma, Italy
- Dipartimento di Fisica, Università di Roma La Sapienza, I-00185 Roma, Italy
| | - A Pilloni
- INFN Sezione di Roma, I-00185 Roma, Italy
- Dipartimento di Fisica, Università di Roma La Sapienza, I-00185 Roma, Italy
| | - G Piredda
- INFN Sezione di Roma, I-00185 Roma, Italy
| | - C Bünger
- Universität Rostock, D-18051 Rostock, Germany
| | - S Dittrich
- Universität Rostock, D-18051 Rostock, Germany
| | - O Grünberg
- Universität Rostock, D-18051 Rostock, Germany
| | - M Heß
- Universität Rostock, D-18051 Rostock, Germany
| | - T Leddig
- Universität Rostock, D-18051 Rostock, Germany
| | - C Voß
- Universität Rostock, D-18051 Rostock, Germany
| | - R Waldi
- Universität Rostock, D-18051 Rostock, Germany
| | - T Adye
- Rutherford Appleton Laboratory, Chilton, Didcot, Oxon OX11 0QX, United Kingdom
| | - F F Wilson
- Rutherford Appleton Laboratory, Chilton, Didcot, Oxon OX11 0QX, United Kingdom
| | - S Emery
- CEA, Irfu, SPP, Centre de Saclay, F-91191 Gif-sur-Yvette, France
| | - G Vasseur
- CEA, Irfu, SPP, Centre de Saclay, F-91191 Gif-sur-Yvette, France
| | - D Aston
- SLAC National Accelerator Laboratory, Stanford, California 94309 USA
| | - C Cartaro
- SLAC National Accelerator Laboratory, Stanford, California 94309 USA
| | - M R Convery
- SLAC National Accelerator Laboratory, Stanford, California 94309 USA
| | - J Dorfan
- SLAC National Accelerator Laboratory, Stanford, California 94309 USA
| | - W Dunwoodie
- SLAC National Accelerator Laboratory, Stanford, California 94309 USA
| | - M Ebert
- SLAC National Accelerator Laboratory, Stanford, California 94309 USA
| | - R C Field
- SLAC National Accelerator Laboratory, Stanford, California 94309 USA
| | - B G Fulsom
- SLAC National Accelerator Laboratory, Stanford, California 94309 USA
| | - M T Graham
- SLAC National Accelerator Laboratory, Stanford, California 94309 USA
| | - C Hast
- SLAC National Accelerator Laboratory, Stanford, California 94309 USA
| | - W R Innes
- SLAC National Accelerator Laboratory, Stanford, California 94309 USA
| | - P Kim
- SLAC National Accelerator Laboratory, Stanford, California 94309 USA
| | - D W G S Leith
- SLAC National Accelerator Laboratory, Stanford, California 94309 USA
| | - S Luitz
- SLAC National Accelerator Laboratory, Stanford, California 94309 USA
| | - D B MacFarlane
- SLAC National Accelerator Laboratory, Stanford, California 94309 USA
| | - D R Muller
- SLAC National Accelerator Laboratory, Stanford, California 94309 USA
| | - H Neal
- SLAC National Accelerator Laboratory, Stanford, California 94309 USA
| | - B N Ratcliff
- SLAC National Accelerator Laboratory, Stanford, California 94309 USA
| | - A Roodman
- SLAC National Accelerator Laboratory, Stanford, California 94309 USA
| | - M K Sullivan
- SLAC National Accelerator Laboratory, Stanford, California 94309 USA
| | - J Va'vra
- SLAC National Accelerator Laboratory, Stanford, California 94309 USA
| | - W J Wisniewski
- SLAC National Accelerator Laboratory, Stanford, California 94309 USA
| | - M V Purohit
- University of South Carolina, Columbia, South Carolina 29208, USA
| | - J R Wilson
- University of South Carolina, Columbia, South Carolina 29208, USA
| | | | - S J Sekula
- Southern Methodist University, Dallas, Texas 75275, USA
| | - M Bellis
- Stanford University, Stanford, California 94305, USA
| | - P R Burchat
- Stanford University, Stanford, California 94305, USA
| | - E M T Puccio
- Stanford University, Stanford, California 94305, USA
| | - M S Alam
- State University of New York, Albany, New York 12222, USA
| | - J A Ernst
- State University of New York, Albany, New York 12222, USA
| | - R Gorodeisky
- School of Physics and Astronomy, Tel Aviv University, Tel Aviv, 69978, Israel
| | - N Guttman
- School of Physics and Astronomy, Tel Aviv University, Tel Aviv, 69978, Israel
| | - D R Peimer
- School of Physics and Astronomy, Tel Aviv University, Tel Aviv, 69978, Israel
| | - A Soffer
- School of Physics and Astronomy, Tel Aviv University, Tel Aviv, 69978, Israel
| | - S M Spanier
- University of Tennessee, Knoxville, Tennessee 37996, USA
| | - J L Ritchie
- University of Texas at Austin, Austin, Texas 78712, USA
| | | | - J M Izen
- University of Texas at Dallas, Richardson, Texas 75083, USA
| | - X C Lou
- University of Texas at Dallas, Richardson, Texas 75083, USA
| | - F Bianchi
- INFN Sezione di Torino, I-10125 Torino, Italy
- Dipartimento di Fisica, Università di Torino, I-10125 Torino, Italy
| | - F De Mori
- INFN Sezione di Torino, I-10125 Torino, Italy
- Dipartimento di Fisica, Università di Torino, I-10125 Torino, Italy
| | - A Filippi
- INFN Sezione di Torino, I-10125 Torino, Italy
| | - D Gamba
- INFN Sezione di Torino, I-10125 Torino, Italy
- Dipartimento di Fisica, Università di Torino, I-10125 Torino, Italy
| | - L Lanceri
- INFN Sezione di Trieste and Dipartimento di Fisica, Università di Trieste, I-34127 Trieste, Italy
| | - L Vitale
- INFN Sezione di Trieste and Dipartimento di Fisica, Università di Trieste, I-34127 Trieste, Italy
| | | | - A Oyanguren
- IFIC, Universitat de Valencia-CSIC, E-46071 Valencia, Spain
| | - J Albert
- University of Victoria, Victoria, British Columbia, V8W 3P6, Canada
| | - A Beaulieu
- University of Victoria, Victoria, British Columbia, V8W 3P6, Canada
| | - F U Bernlochner
- University of Victoria, Victoria, British Columbia, V8W 3P6, Canada
| | - G J King
- University of Victoria, Victoria, British Columbia, V8W 3P6, Canada
| | - R Kowalewski
- University of Victoria, Victoria, British Columbia, V8W 3P6, Canada
| | - T Lueck
- University of Victoria, Victoria, British Columbia, V8W 3P6, Canada
| | - I M Nugent
- University of Victoria, Victoria, British Columbia, V8W 3P6, Canada
| | - J M Roney
- University of Victoria, Victoria, British Columbia, V8W 3P6, Canada
| | - R J Sobie
- Institute of Particle Physics, Victoria, British Columbia, V8W 3P6, Canada
- University of Victoria, Victoria, British Columbia, V8W 3P6, Canada
| | - N Tasneem
- University of Victoria, Victoria, British Columbia, V8W 3P6, Canada
| | - T J Gershon
- Department of Physics, University of Warwick, Coventry CV4 7AL, United Kingdom
| | - P F Harrison
- Department of Physics, University of Warwick, Coventry CV4 7AL, United Kingdom
| | - T E Latham
- Department of Physics, University of Warwick, Coventry CV4 7AL, United Kingdom
| | - R Prepost
- University of Wisconsin, Madison, Wisconsin 53706, USA
| | - S L Wu
- University of Wisconsin, Madison, Wisconsin 53706, USA
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Chowdhury NA, Mannan A, Hasan MM, Mamun AA. Heavy ion-acoustic rogue waves in electron-positron multi-ion plasmas. CHAOS (WOODBURY, N.Y.) 2017; 27:093105. [PMID: 28964149 DOI: 10.1063/1.4985113] [Citation(s) in RCA: 4] [Impact Index Per Article: 0.6] [Reference Citation Analysis] [Abstract] [Track Full Text] [Subscribe] [Scholar Register] [Indexed: 06/07/2023]
Abstract
The nonlinear propagation of heavy-ion-acoustic (HIA) waves (HIAWs) in a four-component multi-ion plasma (containing inertial heavy negative ions and light positive ions, as well as inertialess nonextensive electrons and positrons) has been theoretically investigated. The nonlinear Schrödinger (NLS) equation is derived by employing the reductive perturbation method. It is found that the NLS equation leads to the modulational instability (MI) of HIAWs, and to the formation of HIA rogue waves (HIARWs), which are due to the effects of nonlinearity and dispersion in the propagation of HIAWs. The conditions for the MI of HIAWs and the basic properties of the generated HIARWs are identified. It is observed that the striking features (viz., instability criteria, growth rate of MI, amplitude and width of HIARWs, etc.) of the HIAWs are significantly modified by the effects of nonextensivity of electrons and positrons, the ratio of light positive ion mass to heavy negative ion mass, the ratio of electron number density to light positive ion number density, the ratio of electron temperature to positron temperature, etc. The relevancy of our present investigation to the observations in space (viz., cometary comae and earth's ionosphere) and laboratory (viz., solid-high intense laser plasma interaction experiments) plasmas is pointed out.
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Affiliation(s)
- N A Chowdhury
- Department of Physics, Jahangirnagar University, Savar, Dhaka 1342, Bangladesh
| | - A Mannan
- Department of Physics, Jahangirnagar University, Savar, Dhaka 1342, Bangladesh
| | - M M Hasan
- Department of Physics, Jahangirnagar University, Savar, Dhaka 1342, Bangladesh
| | - A A Mamun
- Department of Physics, Jahangirnagar University, Savar, Dhaka 1342, Bangladesh
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Donato F, Korsmeier M, Di Mauro M. Prescriptions on antiproton cross section data for precise theoretical antiproton flux predictions. Int J Clin Exp Med 2017. [DOI: 10.1103/physrevd.96.043007] [Citation(s) in RCA: 22] [Impact Index Per Article: 3.1] [Reference Citation Analysis] [Track Full Text] [Journal Information] [Subscribe] [Scholar Register] [Indexed: 11/07/2022]
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Gelmini GB. Light weakly interacting massive particles. REPORTS ON PROGRESS IN PHYSICS. PHYSICAL SOCIETY (GREAT BRITAIN) 2017; 80:082201. [PMID: 28612761 DOI: 10.1088/1361-6633/aa6e5c] [Citation(s) in RCA: 1] [Impact Index Per Article: 0.1] [Reference Citation Analysis] [Abstract] [Track Full Text] [Subscribe] [Scholar Register] [Indexed: 06/07/2023]
Abstract
Light weakly interacting massive particles (WIMPs) are dark matter particle candidates with weak scale interaction with the known particles, and mass in the GeV to tens of GeV range. Hints of light WIMPs have appeared in several dark matter searches in the last decade. The unprecedented possible coincidence into tantalizingly close regions of mass and cross section of four separate direct detection experimental hints and a potential indirect detection signal in gamma rays from the galactic center, aroused considerable interest in our field. Even if these hints did not so far result in a discovery, they have had a significant impact in our field. Here we review the evidence for and against light WIMPs as dark matter candidates and discuss future relevant experiments and observations.
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Affiliation(s)
- Graciela B Gelmini
- Department of Physics and Astronomy, University of California, Los Angeles (UCLA), 475 Portola Plaza, Los Angeles, CA 90095, United States of America
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Rogatko M, Wysokiński KI. Viscosity bound for anisotropic superfluids with dark matter sector. Int J Clin Exp Med 2017. [DOI: 10.1103/physrevd.96.026015] [Citation(s) in RCA: 2] [Impact Index Per Article: 0.3] [Reference Citation Analysis] [Track Full Text] [Journal Information] [Subscribe] [Scholar Register] [Indexed: 11/07/2022]
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