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Fransson C, Barlow MJ, Kavanagh PJ, Larsson J, Jones OC, Sargent B, Meixner M, Bouchet P, Temim T, Wright GS, Blommaert JADL, Habel N, Hirschauer AS, Hjorth J, Lenkić L, Tikkanen T, Wesson R, Coulais A, Fox OD, Gastaud R, Glasse A, Jaspers J, Krause O, Lau RM, Nayak O, Rest A, Colina L, van Dishoeck EF, Güdel M, Henning T, Lagage PO, Östlin G, Ray TP, Vandenbussche B. Emission lines due to ionizing radiation from a compact object in the remnant of Supernova 1987A. Science 2024; 383:898-903. [PMID: 38386759 DOI: 10.1126/science.adj5796] [Citation(s) in RCA: 0] [Impact Index Per Article: 0] [Reference Citation Analysis] [Abstract] [Track Full Text] [Journal Information] [Subscribe] [Scholar Register] [Received: 07/06/2023] [Accepted: 01/12/2024] [Indexed: 02/24/2024]
Abstract
The nearby Supernova 1987A was accompanied by a burst of neutrino emission, which indicates that a compact object (a neutron star or black hole) was formed in the explosion. There has been no direct observation of this compact object. In this work, we observe the supernova remnant with JWST spectroscopy, finding narrow infrared emission lines of argon and sulfur. The line emission is spatially unresolved and blueshifted in velocity relative to the supernova rest frame. We interpret the lines as gas illuminated by a source of ionizing photons located close to the center of the expanding ejecta. Photoionization models show that the line ratios are consistent with ionization by a cooling neutron star or a pulsar wind nebula. The velocity shift could be evidence for a neutron star natal kick.
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Affiliation(s)
- C Fransson
- Department of Astronomy, Stockholm University, The Oskar Klein Centre, AlbaNova, SE-106 91 Stockholm, Sweden
| | - M J Barlow
- Department of Physics and Astronomy, University College London, London WC1E 6BT, UK
| | - P J Kavanagh
- Department of Experimental Physics, Maynooth University, Maynooth, County Kildare, Ireland
- Astronomy & Astrophyics Section, School of Cosmic Physics, Dublin Institute for Advanced Studies, Dublin 2, Ireland
| | - J Larsson
- Department of Physics, KTH Royal Institute of Technology, The Oskar Klein Centre, AlbaNova, SE-106 91 Stockholm, Sweden
| | - O C Jones
- UK Astronomy Technology Centre, Royal Observatory, Blackford Hill, Edinburgh EH9 3HJ, UK
| | - B Sargent
- Space Telescope Science Institute, Baltimore, MD 21218, USA
- Department of Physics and Astronomy, The Johns Hopkins University, Baltimore, MD 21218, USA
| | - M Meixner
- Jet Propulsion Laboratory, California Institute of Technology, Pasadena, CA 91109, USA
| | - P Bouchet
- Université Paris-Saclay, Université Paris Cité, Commissariat à l'Énergie Atomique et aux Énergies Alternatives, Centre National de la Recherche Scientifique, Astrophysique Instrumentation Modélisation, Saint Aubin, France
| | - T Temim
- Department of Astrophysical Sciences, Princeton University, Princeton, NJ 08544, USA
| | - G S Wright
- UK Astronomy Technology Centre, Royal Observatory, Blackford Hill, Edinburgh EH9 3HJ, UK
| | - J A D L Blommaert
- Astronomy and Astrophysics Research Group, Department of Physics and Astrophysics, Vrije Universiteit Brussel, B-1050 Brussels, Belgium
| | - N Habel
- Jet Propulsion Laboratory, California Institute of Technology, Pasadena, CA 91109, USA
| | - A S Hirschauer
- Space Telescope Science Institute, Baltimore, MD 21218, USA
| | - J Hjorth
- Dark Cosmology Centre, Niels Bohr Institute, University of Copenhagen, 2200 Copenhagen, Denmark
| | - L Lenkić
- Stratospheric Observatory for Infrared Astronomy Science Center, Universities Space Research Association, NASA Ames Research Center, Moffett Field, CA 94035, USA
| | - T Tikkanen
- School of Physics and Astronomy, Space Research Centre, Space Park Leicester, University of Leicester, Leicester LE4 5SP, UK
| | - R Wesson
- School of Physics and Astronomy, Cardiff University, Cardiff CF24 3AA, UK
| | - A Coulais
- Université Paris-Saclay, Université Paris Cité, Commissariat à l'Énergie Atomique et aux Énergies Alternatives, Centre National de la Recherche Scientifique, Astrophysique Instrumentation Modélisation, Saint Aubin, France
- Laboratoire d'Etudes du Rayonnement et de la Matière en Astrophysique et Atmosphères, Observatoire de Paris, Paris Sciences et Lettres Research University, National Centre for Scientific Research, Sorbonne Université, Paris, France
| | - O D Fox
- Space Telescope Science Institute, Baltimore, MD 21218, USA
| | - R Gastaud
- Université Paris-Saclay, Commissariat à l'Énergie Atomique et aux Énergies Alternatives, Detectors Electronics and Computing for Physics, Gif-sur-Yvette, France
| | - A Glasse
- UK Astronomy Technology Centre, Royal Observatory, Blackford Hill, Edinburgh EH9 3HJ, UK
| | - J Jaspers
- Department of Experimental Physics, Maynooth University, Maynooth, County Kildare, Ireland
- Astronomy & Astrophyics Section, School of Cosmic Physics, Dublin Institute for Advanced Studies, Dublin 2, Ireland
| | - O Krause
- Max-Planck-Institut für Astronomie, D-69117 Heidelberg, Germany
| | - R M Lau
- National Optical-Infrared Astronomy Research Laboratory, National Science Foundation, Tucson, AZ 85719, USA
| | - O Nayak
- NASA Goddard Space Flight Center, Greenbelt, MD 20770, USA
| | - A Rest
- Space Telescope Science Institute, Baltimore, MD 21218, USA
- Department of Physics and Astronomy, The Johns Hopkins University, Baltimore, MD 21218, USA
| | - L Colina
- Centro de Astrobiología, Consejo Superior de Investigaciones Científicas - Instituto Nacional de Técnica Aeroespacial, Torrejón de Ardoz, E-28850, Madrid, Spain
| | - E F van Dishoeck
- Max-Planck Institut für Extraterrestrische Physik, D-85748 Garching, Germany
- Leiden Observatory, 2300 RA Leiden, Netherlands
| | - M Güdel
- Max-Planck-Institut für Astronomie, D-69117 Heidelberg, Germany
- Department of Astrophysics, University of Vienna, A-1180 Vienna, Austria
- Institute for Particle Physics and Astrophysics, Eidgenössische Technische Hochschule Zürich, 8093 Zürich, Switzerland
| | - Th Henning
- Max-Planck-Institut für Astronomie, D-69117 Heidelberg, Germany
| | - P-O Lagage
- Université Paris-Saclay, Université Paris Cité, Commissariat à l'Énergie Atomique et aux Énergies Alternatives, Centre National de la Recherche Scientifique, Astrophysique Instrumentation Modélisation, Saint Aubin, France
| | - G Östlin
- Department of Astronomy, Stockholm University, The Oskar Klein Centre, AlbaNova, SE-106 91 Stockholm, Sweden
| | - T P Ray
- Astronomy & Astrophyics Section, School of Cosmic Physics, Dublin Institute for Advanced Studies, Dublin 2, Ireland
| | - B Vandenbussche
- Institute of Astronomy, Katholieke Universiteit Leuven, 3001 Leuven, Belgium
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2
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Wen AY, Argüelles CA, Kheirandish A, Murase K. Detecting High-Energy Neutrinos from Galactic Supernovae with ATLAS. PHYSICAL REVIEW LETTERS 2024; 132:061001. [PMID: 38394588 DOI: 10.1103/physrevlett.132.061001] [Citation(s) in RCA: 0] [Impact Index Per Article: 0] [Reference Citation Analysis] [Abstract] [Track Full Text] [Subscribe] [Scholar Register] [Received: 09/25/2023] [Accepted: 01/09/2024] [Indexed: 02/25/2024]
Abstract
We show that ATLAS, a collider detector, can measure the flux of high-energy supernova neutrinos, which can be produced from days to months after the explosion. Using Monte Carlo simulations for predicted fluxes, we find at most O(0.1-1) starting events and O(10-100) throughgoing events from a supernova 10 kpc away. Possible Galactic supernovae from Betelgeuse and Eta Carinae are further analyzed as demonstrative examples. We argue that, even with limited statistics, ATLAS has the ability to discriminate among flavors and between neutrinos and antineutrinos, making it a unique neutrino observatory so far unmatched in this capability.
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Affiliation(s)
- Alex Y Wen
- Department of Physics and Laboratory for Particle Physics and Cosmology, Harvard University, Cambridge, Massachusetts 02138, USA
| | - Carlos A Argüelles
- Department of Physics and Laboratory for Particle Physics and Cosmology, Harvard University, Cambridge, Massachusetts 02138, USA
| | - Ali Kheirandish
- Department of Physics and Astronomy, University of Nevada, Las Vegas, Nevada 89154, USA
- Nevada Center for Astrophysics, University of Nevada, Las Vegas, Nevada 89154, USA
| | - Kohta Murase
- Department of Physics, Department of Astronomy and Astrophysics, and Center for Multimessenger Astrophysics, Institute for Gravitation and the Cosmos, The Pennsylvania State University, University Park, Pennsylvania 16802, USA
- School of Natural Sciences, Institute for Advanced Study, Princeton, New Jersey 08540, USA
- Center for Gravitational Physics and Quantum Information, Yukawa Institute for Theoretical Physics, Kyoto, Kyoto 16802, Japan
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3
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YAMADA S, NAGAKURA H, AKAHO R, HARADA A, FURUSAWA S, IWAKAMI W, OKAWA H, MATSUFURU H, SUMIYOSHI K. Physical mechanism of core-collapse supernovae that neutrinos drive. PROCEEDINGS OF THE JAPAN ACADEMY. SERIES B, PHYSICAL AND BIOLOGICAL SCIENCES 2024; 100:190-233. [PMID: 38462501 PMCID: PMC11105976 DOI: 10.2183/pjab.100.015] [Citation(s) in RCA: 0] [Impact Index Per Article: 0] [Reference Citation Analysis] [Abstract] [Key Words] [MESH Headings] [Track Full Text] [Subscribe] [Scholar Register] [Received: 02/05/2023] [Accepted: 12/05/2023] [Indexed: 03/12/2024]
Abstract
The current understanding of the mechanism of core-collapse supernovae (CCSNe), one of the most energetic events in the universe associated with the death of massive stars and the main formation channel of compact objects such as neutron stars and black holes, is reviewed for broad readers from different disciplines of science who may not be familiar with the object. Therefore, we emphasize the physical aspects than the results of individual model simulations, although large-scale high-fidelity simulations have played the most important roles in the progress we have witnessed in the past few decades. It is now believed that neutrinos are the most important agent in producing the commonest type of CCSNe. The so-called neutrino-heating mechanism will be the focus of this review and its crucial ingredients in micro- and macrophysics and in numerics will be explained one by one. We will also try to elucidate the remaining issues.
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Affiliation(s)
- Shoichi YAMADA
- Department of Physics, Faculty of Science and Engineering, Waseda University, Tokyo, Japan
- Research Institute for Science and Engineering, Waseda University, Tokyo, Japan
| | - Hiroki NAGAKURA
- National Astronomical Observatory of Japan, Mitaka, Tokyo, Japan
| | - Ryuichiro AKAHO
- Department of Physics, Faculty of Science and Engineering, Waseda University, Tokyo, Japan
| | - Akira HARADA
- Interdisciplinary Theoretical and Mathematical Sciences Program (iTHEMS), RIKEN, Wako, Saitama, Japan
| | - Shun FURUSAWA
- College of Science and Engineering, Kanto Gakuin University, Yokohama, Kanagawa, Japan
| | - Wakana IWAKAMI
- Department of Physics, Faculty of Science and Engineering, Waseda University, Tokyo, Japan
| | - Hirotada OKAWA
- Waseda Institute for Advanced Study, Waseda University, Tokyo, Japan
| | - Hideo MATSUFURU
- High Energy Accelerator Research Organization (KEK), Tsukuba, Ibaraki, Japan
| | - Kohsuke SUMIYOSHI
- National Institute of Technology, Numazu College, Numazu, Shizuoka, Japan
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4
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Chang PW, Esteban I, Beacom JF, Thompson TA, Hirata CM. Toward Powerful Probes of Neutrino Self-Interactions in Supernovae. PHYSICAL REVIEW LETTERS 2023; 131:071002. [PMID: 37656847 DOI: 10.1103/physrevlett.131.071002] [Citation(s) in RCA: 1] [Impact Index Per Article: 1.0] [Reference Citation Analysis] [Abstract] [Track Full Text] [Subscribe] [Scholar Register] [Received: 07/11/2022] [Revised: 11/02/2022] [Accepted: 06/23/2023] [Indexed: 09/03/2023]
Abstract
Neutrinos remain mysterious. As an example, enhanced self-interactions (νSI), which would have broad implications, are allowed. At the high neutrino densities within core-collapse supernovae, νSI should be important, but robust observables have been lacking. We show that νSI make neutrinos form a tightly coupled fluid that expands under relativistic hydrodynamics. The outflow becomes either a burst or a steady-state wind; which occurs here is uncertain. Though the diffusive environment where neutrinos are produced may make a wind more likely, further work is needed to determine when each case is realized. In the burst-outflow case, νSI increase the duration of the neutrino signal, and even a simple analysis of SN 1987A data has powerful sensitivity. For the wind-outflow case, we outline several promising ideas that may lead to new observables. Combined, these results are important steps toward solving the 35-year-old puzzle of how νSI affect supernovae.
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Affiliation(s)
- Po-Wen Chang
- Center for Cosmology and AstroParticle Physics (CCAPP), Ohio State University, Columbus, Ohio 43210, USA
- Department of Physics, Ohio State University, Columbus, Ohio 43210, USA
| | - Ivan Esteban
- Center for Cosmology and AstroParticle Physics (CCAPP), Ohio State University, Columbus, Ohio 43210, USA
- Department of Physics, Ohio State University, Columbus, Ohio 43210, USA
| | - John F Beacom
- Center for Cosmology and AstroParticle Physics (CCAPP), Ohio State University, Columbus, Ohio 43210, USA
- Department of Physics, Ohio State University, Columbus, Ohio 43210, USA
- Department of Astronomy, Ohio State University, Columbus, Ohio 43210, USA
| | - Todd A Thompson
- Center for Cosmology and AstroParticle Physics (CCAPP), Ohio State University, Columbus, Ohio 43210, USA
- Department of Physics, Ohio State University, Columbus, Ohio 43210, USA
- Department of Astronomy, Ohio State University, Columbus, Ohio 43210, USA
| | - Christopher M Hirata
- Center for Cosmology and AstroParticle Physics (CCAPP), Ohio State University, Columbus, Ohio 43210, USA
- Department of Physics, Ohio State University, Columbus, Ohio 43210, USA
- Department of Astronomy, Ohio State University, Columbus, Ohio 43210, USA
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5
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Aydiner E. Anomalous cyclic in the neutrino oscillations. Sci Rep 2023; 13:12651. [PMID: 37542165 PMCID: PMC10403527 DOI: 10.1038/s41598-023-39871-3] [Citation(s) in RCA: 1] [Impact Index Per Article: 1.0] [Reference Citation Analysis] [Abstract] [Key Words] [Track Full Text] [Journal Information] [Subscribe] [Scholar Register] [Received: 01/12/2023] [Accepted: 08/01/2023] [Indexed: 08/06/2023] Open
Abstract
Neutrino physics is one of the most important topics in particle physics and cosmology. As it is known, neutrinos are weakly interacting fundamental particles with chargeless and very small masses. One of the most characteristic features of the neutrino that make a difference from other elementary particles is that it oscillates between the mass and flavour eigenstates. Due to these oscillations, neutrinos change from one flavour to another. So far in theory the possible effects of deformed space-time effects on oscillation have not been considered. In this study, we show for the first time that a deformed space-time metric will lead to fractional dynamics between mass and flavour changes and therefore cause a phase shift in the oscillation period. We also shortly discuss the possible relation between anomalous cyclic and relic neutrinos. The modification in the oscillation probabilities due to the studied effect in this work could be seen using relic neutrinos.
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Affiliation(s)
- E Aydiner
- Department of Physics, Faculty of Science, Istanbul University, 34134, Istanbul, Turkey.
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6
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Abreu H, Anders J, Antel C, Ariga A, Ariga T, Atkinson J, Bernlochner FU, Blesgen T, Boeckh T, Boyd J, Brenner L, Cadoux F, Casper DW, Cavanagh C, Chen X, Coccaro A, Desai A, Dmitrievsky S, D'Onofrio M, Favre Y, Fellers D, Feng JL, Fenoglio CA, Ferrere D, Gibson S, Gonzalez-Sevilla S, Gornushkin Y, Gwilliam C, Hayakawa D, Hsu SC, Hu Z, Iacobucci G, Inada T, Jakobsen S, Joos H, Kajomovitz E, Kawahara H, Keyken A, Kling F, Köck D, Kose U, Kotitsa R, Kuehn S, Lefebvre H, Levinson L, Li K, Liu J, MacDonald J, Magliocca C, Martinelli F, McFayden J, Milanesio M, Mladenov D, Moretti T, Munker M, Nakamura M, Nakano T, Nessi M, Neuhaus F, Nevay L, Otono H, Pang H, Paolozzi L, Petersen B, Pietropaolo F, Prim M, Queitsch-Maitland M, Resnati F, Rokujo H, Ruiz-Choliz E, Sabater-Iglesias J, Sato O, Scampoli P, Schmieden K, Schott M, Sfyrla A, Shively S, Takubo Y, Tarannum N, Theiner O, Torrence E, Tufanli S, Vasina S, Vormwald B, Wang D, Welch E, Zambito S. First Direct Observation of Collider Neutrinos with FASER at the LHC. PHYSICAL REVIEW LETTERS 2023; 131:031801. [PMID: 37540863 DOI: 10.1103/physrevlett.131.031801] [Citation(s) in RCA: 1] [Impact Index Per Article: 1.0] [Reference Citation Analysis] [Abstract] [Track Full Text] [Subscribe] [Scholar Register] [Received: 03/24/2023] [Accepted: 05/08/2023] [Indexed: 08/06/2023]
Abstract
We report the first direct observation of neutrino interactions at a particle collider experiment. Neutrino candidate events are identified in a 13.6 TeV center-of-mass energy pp collision dataset of 35.4 fb^{-1} using the active electronic components of the FASER detector at the Large Hadron Collider. The candidates are required to have a track propagating through the entire length of the FASER detector and be consistent with a muon neutrino charged-current interaction. We infer 153_{-13}^{+12} neutrino interactions with a significance of 16 standard deviations above the background-only hypothesis. These events are consistent with the characteristics expected from neutrino interactions in terms of secondary particle production and spatial distribution, and they imply the observation of both neutrinos and anti-neutrinos with an incident neutrino energy of significantly above 200 GeV.
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Affiliation(s)
- Henso Abreu
- Department of Physics and Astronomy, Technion-Israel Institute of Technology, Haifa 32000, Israel
| | | | - Claire Antel
- Département de Physique Nucléaire et Corpusculaire, University of Geneva, CH-1211 Geneva 4, Switzerland
| | - Akitaka Ariga
- Albert Einstein Center for Fundamental Physics, Laboratory for High Energy Physics, University of Bern, Sidlerstrasse 5, CH-3012 Bern, Switzerland
- Department of Physics, Chiba University, 1-33 Yayoi-cho Inage-ku, 263-8522 Chiba, Japan
| | - Tomoko Ariga
- Kyushu University, Nishi-ku, 819-0395 Fukuoka, Japan
| | - Jeremy Atkinson
- Albert Einstein Center for Fundamental Physics, Laboratory for High Energy Physics, University of Bern, Sidlerstrasse 5, CH-3012 Bern, Switzerland
| | | | - Tobias Blesgen
- Universität Bonn, Regina-Pacis-Weg 3, D-53113 Bonn, Germany
| | - Tobias Boeckh
- Universität Bonn, Regina-Pacis-Weg 3, D-53113 Bonn, Germany
| | | | - Lydia Brenner
- Nikhef National Institute for Subatomic Physics, Science Park 105, 1098 XG Amsterdam, Netherlands
| | - Franck Cadoux
- Département de Physique Nucléaire et Corpusculaire, University of Geneva, CH-1211 Geneva 4, Switzerland
| | - David W Casper
- Department of Physics and Astronomy, University of California, Irvine, California 92697-4575, USA
| | | | - Xin Chen
- Department of Physics, Tsinghua University, Beijing, China
| | - Andrea Coccaro
- INFN Sezione di Genova, Via Dodecaneso, 33-16146, Genova, Italy
| | - Ansh Desai
- University of Oregon, Eugene, Oregon 97403, USA
| | - Sergey Dmitrievsky
- Affiliated with an international laboratory covered by a cooperation agreement with CERN
| | | | - Yannick Favre
- Département de Physique Nucléaire et Corpusculaire, University of Geneva, CH-1211 Geneva 4, Switzerland
| | | | - Jonathan L Feng
- Department of Physics and Astronomy, University of California, Irvine, California 92697-4575, USA
| | - Carlo Alberto Fenoglio
- Département de Physique Nucléaire et Corpusculaire, University of Geneva, CH-1211 Geneva 4, Switzerland
| | - Didier Ferrere
- Département de Physique Nucléaire et Corpusculaire, University of Geneva, CH-1211 Geneva 4, Switzerland
| | - Stephen Gibson
- Royal Holloway, University of London, Egham TW20 0EX, United Kingdom
| | - Sergio Gonzalez-Sevilla
- Département de Physique Nucléaire et Corpusculaire, University of Geneva, CH-1211 Geneva 4, Switzerland
| | - Yuri Gornushkin
- Affiliated with an international laboratory covered by a cooperation agreement with CERN
| | - Carl Gwilliam
- University of Liverpool, Liverpool L69 3BX, United Kingdom
| | - Daiki Hayakawa
- Department of Physics, Chiba University, 1-33 Yayoi-cho Inage-ku, 263-8522 Chiba, Japan
| | - Shih-Chieh Hsu
- Department of Physics, University of Washington, PO Box 351560, Seattle, Washington 98195-1460, USA
| | - Zhen Hu
- Department of Physics, Tsinghua University, Beijing, China
| | - Giuseppe Iacobucci
- Département de Physique Nucléaire et Corpusculaire, University of Geneva, CH-1211 Geneva 4, Switzerland
| | - Tomohiro Inada
- Department of Physics, Tsinghua University, Beijing, China
| | | | - Hans Joos
- CERN, CH-1211 Geneva 23, Switzerland
- II. Physikalisches Institut, Universität Göttingen, Göttingen, Germany
| | - Enrique Kajomovitz
- Department of Physics and Astronomy, Technion-Israel Institute of Technology, Haifa 32000, Israel
| | | | - Alex Keyken
- Royal Holloway, University of London, Egham TW20 0EX, United Kingdom
| | - Felix Kling
- Deutsches Elektronen-Synchrotron DESY, Notkestr. 85, 22607 Hamburg, Germany
| | | | - Umut Kose
- CERN, CH-1211 Geneva 23, Switzerland
| | | | | | - Helena Lefebvre
- Royal Holloway, University of London, Egham TW20 0EX, United Kingdom
| | - Lorne Levinson
- Department of Particle Physics and Astrophysics, Weizmann Institute of Science, Rehovot 76100, Israel
| | - Ke Li
- Department of Physics, University of Washington, PO Box 351560, Seattle, Washington 98195-1460, USA
| | - Jinfeng Liu
- Department of Physics, Tsinghua University, Beijing, China
| | | | - Chiara Magliocca
- Département de Physique Nucléaire et Corpusculaire, University of Geneva, CH-1211 Geneva 4, Switzerland
| | - Fulvio Martinelli
- Département de Physique Nucléaire et Corpusculaire, University of Geneva, CH-1211 Geneva 4, Switzerland
| | - Josh McFayden
- Department of Physics and Astronomy, University of Sussex, Sussex House, Falmer, Brighton BN1 9RH, United Kingdom
| | - Matteo Milanesio
- Département de Physique Nucléaire et Corpusculaire, University of Geneva, CH-1211 Geneva 4, Switzerland
| | | | - Théo Moretti
- Département de Physique Nucléaire et Corpusculaire, University of Geneva, CH-1211 Geneva 4, Switzerland
| | - Magdalena Munker
- Département de Physique Nucléaire et Corpusculaire, University of Geneva, CH-1211 Geneva 4, Switzerland
| | | | | | - Marzio Nessi
- CERN, CH-1211 Geneva 23, Switzerland
- Département de Physique Nucléaire et Corpusculaire, University of Geneva, CH-1211 Geneva 4, Switzerland
| | | | - Laurie Nevay
- CERN, CH-1211 Geneva 23, Switzerland
- Royal Holloway, University of London, Egham TW20 0EX, United Kingdom
| | | | - Hao Pang
- Department of Physics, Tsinghua University, Beijing, China
| | - Lorenzo Paolozzi
- CERN, CH-1211 Geneva 23, Switzerland
- Département de Physique Nucléaire et Corpusculaire, University of Geneva, CH-1211 Geneva 4, Switzerland
| | | | | | - Markus Prim
- Universität Bonn, Regina-Pacis-Weg 3, D-53113 Bonn, Germany
| | - Michaela Queitsch-Maitland
- University of Manchester, School of Physics and Astronomy, Schuster Building, Oxford Rd, Manchester M13 9PL, United Kingdom
| | | | - Hiroki Rokujo
- Nagoya University, Furo-cho, Chikusa-ku, Nagoya 464-8602, Japan
| | | | - Jorge Sabater-Iglesias
- Département de Physique Nucléaire et Corpusculaire, University of Geneva, CH-1211 Geneva 4, Switzerland
| | - Osamu Sato
- Nagoya University, Furo-cho, Chikusa-ku, Nagoya 464-8602, Japan
| | - Paola Scampoli
- Albert Einstein Center for Fundamental Physics, Laboratory for High Energy Physics, University of Bern, Sidlerstrasse 5, CH-3012 Bern, Switzerland
- Dipartimento di Fisica "Ettore Pancini", Università di Napoli Federico II, Complesso Universitario di Monte S. Angelo, I-80126 Napoli, Italy
| | | | | | - Anna Sfyrla
- Département de Physique Nucléaire et Corpusculaire, University of Geneva, CH-1211 Geneva 4, Switzerland
| | - Savannah Shively
- Department of Physics and Astronomy, University of California, Irvine, California 92697-4575, USA
| | - Yosuke Takubo
- Institute of Particle and Nuclear Studies, KEK, Oho 1-1, Tsukuba, Ibaraki 305-0801, Japan
| | - Noshin Tarannum
- Département de Physique Nucléaire et Corpusculaire, University of Geneva, CH-1211 Geneva 4, Switzerland
| | - Ondrej Theiner
- Département de Physique Nucléaire et Corpusculaire, University of Geneva, CH-1211 Geneva 4, Switzerland
| | | | | | - Svetlana Vasina
- Affiliated with an international laboratory covered by a cooperation agreement with CERN
| | | | - Di Wang
- Department of Physics, Tsinghua University, Beijing, China
| | - Eli Welch
- Department of Physics and Astronomy, University of California, Irvine, California 92697-4575, USA
| | - Stefano Zambito
- Département de Physique Nucléaire et Corpusculaire, University of Geneva, CH-1211 Geneva 4, Switzerland
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7
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Fiorillo DFG, Raffelt GG, Vitagliano E. Strong Supernova 1987A Constraints on Bosons Decaying to Neutrinos. PHYSICAL REVIEW LETTERS 2023; 131:021001. [PMID: 37505964 DOI: 10.1103/physrevlett.131.021001] [Citation(s) in RCA: 2] [Impact Index Per Article: 2.0] [Reference Citation Analysis] [Abstract] [Track Full Text] [Subscribe] [Scholar Register] [Received: 09/28/2022] [Revised: 01/17/2023] [Accepted: 06/21/2023] [Indexed: 07/30/2023]
Abstract
Majoron-like bosons would emerge from a supernova (SN) core by neutrino coalescence of the form νν→ϕ and ν[over ¯]ν[over ¯]→ϕ with 100-MeV-range energies. Subsequent decays to (anti)neutrinos of all flavors provide a flux component with energies much larger than the usual flux from the "neutrino sphere." The absence of 100-MeV-range events in the Kamiokande-II and Irvine-Michigan-Brookhaven signal of SN 1987A implies that less than 1% of the total energy was thus emitted and provides the strongest constraint on the Majoron-neutrino coupling of g≲10^{-9} MeV/m_{ϕ} for 100 eV≲m_{ϕ}≲100 MeV. It is straightforward to extend our new argument to other hypothetical feebly interacting particles.
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Affiliation(s)
- Damiano F G Fiorillo
- Niels Bohr International Academy, Niels Bohr Institute, University of Copenhagen, 2100 Copenhagen, Denmark
| | - Georg G Raffelt
- Max-Planck-Institut für Physik (Werner-Heisenberg-Institut), Föhringer Ring 6, 80805 München, Germany
| | - Edoardo Vitagliano
- Department of Physics and Astronomy, University of California, Los Angeles, California 90095-1547, USA
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8
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Beeman JW, Benato G, Bucci C, Canonica L, Carniti P, Celi E, Clemenza M, D'Addabbo A, Danevich FA, Di Domizio S, Di Lorenzo S, Dubovik OM, Ferreiro Iachellini N, Ferroni F, Fiorini E, Fu S, Garai A, Ghislandi S, Gironi L, Gorla P, Gotti C, Guillaumon PV, Helis DL, Kovtun GP, Mancuso M, Marini L, Olmi M, Pagnanini L, Pattavina L, Pessina G, Petricca F, Pirro S, Pozzi S, Puiu A, Quitadamo S, Rothe J, Scherban AP, Schönert S, Solopikhin DA, Strauss R, Tarabini E, Tretyak VI, Tupitsyna IA, Wagner V. Characterization of a kg-scale archaeological lead-based PbWO 4 cryogenic detector for the RES-NOVA experiment. Appl Radiat Isot 2023; 194:110704. [PMID: 36731392 DOI: 10.1016/j.apradiso.2023.110704] [Citation(s) in RCA: 0] [Impact Index Per Article: 0] [Reference Citation Analysis] [Abstract] [Key Words] [Track Full Text] [Journal Information] [Subscribe] [Scholar Register] [Received: 05/29/2022] [Revised: 01/21/2023] [Accepted: 01/26/2023] [Indexed: 01/30/2023]
Abstract
Core-collapse Supernovae (SNe) are one of the most energetic events in the Universe, during which almost all the star's binding energy is released in the form of neutrinos. These particles are direct probes of the processes occurring in the stellar core and provide unique insights into the gravitational collapse. RES-NOVA will revolutionize how we detect neutrinos from astrophysical sources, by deploying the first ton-scale array of cryogenic detectors made from archaeological lead. Pb offers the highest neutrino interaction cross-section via coherent elastic neutrino-nucleus scattering (CEνNS). Such process will enable RES-NOVA to be equally sensitive to all neutrino flavours. For the first time, we propose the use archaeological Pb as sensitive target material in order to achieve an ultra-low background level in the region of interest (O(1 keV)). All these features make possible the deployment of the first cm-scale neutrino telescope for the investigation of astrophysical sources. In this contribution, we will characterize the radiopurity level and the performance of a small-scale proof-of-principle detector of RES-NOVA, consisting in a PbWO4 crystal made from archaeological-Pb operated as cryogenic detector.
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Affiliation(s)
- J W Beeman
- Lawrence Berkeley National Laboratory, Berkeley, 94720, CA, USA
| | - G Benato
- Laboratori Nazionali del Gran Sasso, Via G. Acitelli 22, Assergi, 67100, IT, Italy
| | - C Bucci
- Laboratori Nazionali del Gran Sasso, Via G. Acitelli 22, Assergi, 67100, IT, Italy
| | - L Canonica
- Max-Planck-Institut für Physik, Föhringer Ring 6, München, DE-80805, Germany
| | - P Carniti
- Dipartimento di Fisica, Università di Milano - Bicocca, Piazza della Scienza 3, Milano, I-20126, IT, Italy; INFN Sezione di Milano - Bicocca, Piazza della Scienza 3, Milano, I-20126, IT, Italy
| | - E Celi
- Laboratori Nazionali del Gran Sasso, Via G. Acitelli 22, Assergi, 67100, IT, Italy; Gran Sasso Science Institute, Viale F. Crespi 7, L'Aquila, 67100, IT, Italy
| | - M Clemenza
- INFN Sezione di Milano - Bicocca, Piazza della Scienza 3, Milano, I-20126, IT, Italy
| | - A D'Addabbo
- Laboratori Nazionali del Gran Sasso, Via G. Acitelli 22, Assergi, 67100, IT, Italy
| | - F A Danevich
- Institute for Nuclear Research of NASU, Kyiv, 03028, Ukraine
| | - S Di Domizio
- INFN Sezione di Genova and Università di Genova, Via Dodecaneso 33, Genova, I-16146, IT, Italy
| | - S Di Lorenzo
- Laboratori Nazionali del Gran Sasso, Via G. Acitelli 22, Assergi, 67100, IT, Italy
| | - O M Dubovik
- Institute of Scintillation Materials of NASU, Kharkiv, 61072, Ukraine
| | | | - F Ferroni
- Gran Sasso Science Institute, Viale F. Crespi 7, L'Aquila, 67100, IT, Italy; INFN Sezione di Roma-1, P.le Aldo Moro 2, Roma, I-00185, IT, Italy
| | - E Fiorini
- Dipartimento di Fisica, Università di Milano - Bicocca, Piazza della Scienza 3, Milano, I-20126, IT, Italy; INFN Sezione di Milano - Bicocca, Piazza della Scienza 3, Milano, I-20126, IT, Italy
| | - S Fu
- Laboratori Nazionali del Gran Sasso, Via G. Acitelli 22, Assergi, 67100, IT, Italy
| | - A Garai
- Max-Planck-Institut für Physik, Föhringer Ring 6, München, DE-80805, Germany
| | - S Ghislandi
- Laboratori Nazionali del Gran Sasso, Via G. Acitelli 22, Assergi, 67100, IT, Italy; Gran Sasso Science Institute, Viale F. Crespi 7, L'Aquila, 67100, IT, Italy
| | - L Gironi
- Dipartimento di Fisica, Università di Milano - Bicocca, Piazza della Scienza 3, Milano, I-20126, IT, Italy; INFN Sezione di Milano - Bicocca, Piazza della Scienza 3, Milano, I-20126, IT, Italy
| | - P Gorla
- Laboratori Nazionali del Gran Sasso, Via G. Acitelli 22, Assergi, 67100, IT, Italy
| | - C Gotti
- Dipartimento di Fisica, Università di Milano - Bicocca, Piazza della Scienza 3, Milano, I-20126, IT, Italy; INFN Sezione di Milano - Bicocca, Piazza della Scienza 3, Milano, I-20126, IT, Italy
| | - P V Guillaumon
- Laboratori Nazionali del Gran Sasso, Via G. Acitelli 22, Assergi, 67100, IT, Italy
| | - D L Helis
- Laboratori Nazionali del Gran Sasso, Via G. Acitelli 22, Assergi, 67100, IT, Italy; Gran Sasso Science Institute, Viale F. Crespi 7, L'Aquila, 67100, IT, Italy
| | - G P Kovtun
- National Science Center 'Kharkiv Institute of Physics and Technology', Kharkiv, 61108, Ukraine
| | - M Mancuso
- Max-Planck-Institut für Physik, Föhringer Ring 6, München, DE-80805, Germany
| | - L Marini
- Laboratori Nazionali del Gran Sasso, Via G. Acitelli 22, Assergi, 67100, IT, Italy; Gran Sasso Science Institute, Viale F. Crespi 7, L'Aquila, 67100, IT, Italy
| | - M Olmi
- Laboratori Nazionali del Gran Sasso, Via G. Acitelli 22, Assergi, 67100, IT, Italy
| | - L Pagnanini
- Laboratori Nazionali del Gran Sasso, Via G. Acitelli 22, Assergi, 67100, IT, Italy; Gran Sasso Science Institute, Viale F. Crespi 7, L'Aquila, 67100, IT, Italy
| | - L Pattavina
- Laboratori Nazionali del Gran Sasso, Via G. Acitelli 22, Assergi, 67100, IT, Italy; Technical University of Munich, JamesFranckStrasse 1, Garching, 85748, DE, Germany.
| | - G Pessina
- INFN Sezione di Milano - Bicocca, Piazza della Scienza 3, Milano, I-20126, IT, Italy
| | - F Petricca
- Max-Planck-Institut für Physik, Föhringer Ring 6, München, DE-80805, Germany
| | - S Pirro
- Laboratori Nazionali del Gran Sasso, Via G. Acitelli 22, Assergi, 67100, IT, Italy
| | - S Pozzi
- Dipartimento di Fisica, Università di Milano - Bicocca, Piazza della Scienza 3, Milano, I-20126, IT, Italy; INFN Sezione di Milano - Bicocca, Piazza della Scienza 3, Milano, I-20126, IT, Italy
| | - A Puiu
- Laboratori Nazionali del Gran Sasso, Via G. Acitelli 22, Assergi, 67100, IT, Italy; Gran Sasso Science Institute, Viale F. Crespi 7, L'Aquila, 67100, IT, Italy
| | - S Quitadamo
- Laboratori Nazionali del Gran Sasso, Via G. Acitelli 22, Assergi, 67100, IT, Italy; Gran Sasso Science Institute, Viale F. Crespi 7, L'Aquila, 67100, IT, Italy.
| | - J Rothe
- Technical University of Munich, JamesFranckStrasse 1, Garching, 85748, DE, Germany
| | - A P Scherban
- National Science Center 'Kharkiv Institute of Physics and Technology', Kharkiv, 61108, Ukraine
| | - S Schönert
- Technical University of Munich, JamesFranckStrasse 1, Garching, 85748, DE, Germany
| | - D A Solopikhin
- National Science Center 'Kharkiv Institute of Physics and Technology', Kharkiv, 61108, Ukraine
| | - R Strauss
- Technical University of Munich, JamesFranckStrasse 1, Garching, 85748, DE, Germany
| | - E Tarabini
- INFN Sezione di Milano - Bicocca, Piazza della Scienza 3, Milano, I-20126, IT, Italy
| | - V I Tretyak
- Institute for Nuclear Research of NASU, Kyiv, 03028, Ukraine
| | - I A Tupitsyna
- Institute of Scintillation Materials of NASU, Kharkiv, 61072, Ukraine
| | - V Wagner
- Technical University of Munich, JamesFranckStrasse 1, Garching, 85748, DE, Germany
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Betranhandy A, O’Connor E. Neutrino driven explosions aided by axion cooling in multidimensional simulations of core-collapse supernovae. Int J Clin Exp Med 2022. [DOI: 10.1103/physrevd.106.063019] [Citation(s) in RCA: 0] [Impact Index Per Article: 0] [Reference Citation Analysis] [Track Full Text] [Journal Information] [Subscribe] [Scholar Register] [Indexed: 11/07/2022]
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10
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Pompa F, Capozzi F, Mena O, Sorel M. Absolute ν Mass Measurement with the DUNE Experiment. PHYSICAL REVIEW LETTERS 2022; 129:121802. [PMID: 36179167 DOI: 10.1103/physrevlett.129.121802] [Citation(s) in RCA: 0] [Impact Index Per Article: 0] [Reference Citation Analysis] [Abstract] [Track Full Text] [Subscribe] [Scholar Register] [Received: 03/23/2022] [Revised: 07/18/2022] [Accepted: 08/12/2022] [Indexed: 06/16/2023]
Abstract
Time of flight delay in the supernova neutrino signal offers a unique tool to set model-independent constraints on the absolute neutrino mass. The presence of a sharp time structure during a first emission phase, the so-called neutronization burst in the electron neutrino flavor time distribution, makes this channel a very powerful one. Large liquid argon underground detectors will provide precision measurements of the time dependence of the electron neutrino fluxes. We derive here a new ν mass sensitivity attainable at the future DUNE far detector from a future supernova collapse in our galactic neighborhood, finding a sub-eV reach under favorable scenarios. These values are competitive with those expected for laboratory direct neutrino mass searches.
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Affiliation(s)
- Federica Pompa
- Instituto de Física Corpuscular (IFIC), University of Valencia-CSIC, Parc Científic UV, c/ Catedrático José Beltrán 2, E-46980 Paterna, Spain
| | - Francesco Capozzi
- Instituto de Física Corpuscular (IFIC), University of Valencia-CSIC, Parc Científic UV, c/ Catedrático José Beltrán 2, E-46980 Paterna, Spain
| | - Olga Mena
- Instituto de Física Corpuscular (IFIC), University of Valencia-CSIC, Parc Científic UV, c/ Catedrático José Beltrán 2, E-46980 Paterna, Spain
| | - Michel Sorel
- Instituto de Física Corpuscular (IFIC), University of Valencia-CSIC, Parc Científic UV, c/ Catedrático José Beltrán 2, E-46980 Paterna, Spain
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11
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Bhattacharjee P, Bandyopadhyay A, Chakraborty S, Ghosh S, Kar K, Saha S. Inelastic charged-current interactions of supernova neutrinos in two-phase liquid xenon dark matter detectors. Int J Clin Exp Med 2022. [DOI: 10.1103/physrevd.106.043029] [Citation(s) in RCA: 0] [Impact Index Per Article: 0] [Reference Citation Analysis] [Track Full Text] [Journal Information] [Subscribe] [Scholar Register] [Indexed: 11/07/2022]
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12
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Kubota S, Ho J, McDonald A, Tata N, Asaadi J, Guenette R, Battat J, Braga D, Demarteau M, Djurcic Z, Febbraro M, Gramellini E, Kohani S, Mauger C, Mei Y, Newcomer F, Nishimura K, Nygren D, Van Berg R, Varner G, Woodworth K. Enhanced low-energy supernova burst detection in large liquid argon time projection chambers enabled by Q-Pix. Int J Clin Exp Med 2022. [DOI: 10.1103/physrevd.106.032011] [Citation(s) in RCA: 0] [Impact Index Per Article: 0] [Reference Citation Analysis] [Track Full Text] [Journal Information] [Subscribe] [Scholar Register] [Indexed: 11/07/2022]
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13
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A Multidimensional Multicomponent Gas Dynamic with the Neutrino Transfer in Gravitational Collapse. UNIVERSE 2022. [DOI: 10.3390/universe8070372] [Citation(s) in RCA: 0] [Impact Index Per Article: 0] [Reference Citation Analysis] [Abstract] [Track Full Text] [Subscribe] [Scholar Register] [Indexed: 02/04/2023]
Abstract
The self-consistent problem of gravitational collapse is solved using 2D gas dynamics with taking into account the neutrino transfer in the flux-limited diffusion approximation. Neutrino are described by spectral energy density, and weak interaction includes a simplified physical model of neutrino interactions with nucleons. I investigate convection on the stage of the collapse and then in the center of the core, where the unstable entropy profile was probably formed. It is shown that convection has large scale. Convection appears only in the semitransparent region near the neutrinosphere due to non-equilibrium nonreversible neutronization. Convection increases the energy of emitted neutrino up to 15÷18 MeV. The obtained neutrino spectrum is important for the registration of low-energy neutrinos from a supernova.
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14
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Suliga AM, Beacom JF, Tamborra I. Towards probing the diffuse supernova neutrino background in all flavors. Int J Clin Exp Med 2022. [DOI: 10.1103/physrevd.105.043008] [Citation(s) in RCA: 3] [Impact Index Per Article: 1.5] [Reference Citation Analysis] [Track Full Text] [Journal Information] [Subscribe] [Scholar Register] [Indexed: 11/06/2022]
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15
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Searches for Violation of CPT Symmetry and Lorentz Invariance with Astrophysical Neutrinos. UNIVERSE 2022. [DOI: 10.3390/universe8010042] [Citation(s) in RCA: 0] [Impact Index Per Article: 0] [Reference Citation Analysis] [Abstract] [Track Full Text] [Subscribe] [Scholar Register] [Indexed: 01/27/2023]
Abstract
Neutrinos are a powerful tool for searching physics beyond the standard model of elementary particles. In this review, we present the status of the research on charge-parity-time (CPT) symmetry and Lorentz invariance violations using neutrinos emitted from the collapse of stars such as supernovae and other astrophysical environments, such as gamma-ray bursts. Particularly, supernova neutrino fluxes may provide precious information because all neutrino and antineutrino flavors are emitted during a burst of tens of seconds. Models of quantum gravity may allow the violation of Lorentz invariance and possibly of CPT symmetry. Violation of Lorentz invariance may cause a modification of the dispersion relation and, therefore, in the neutrino group velocity as well in the neutrino wave packet. These changes can affect the arrival time signal registered in astrophysical neutrino detectors. Direction or time-dependent oscillation probabilities and anisotropy of the neutrino velocity are manifestations of the same kind of new physics. CPT violation, on the other hand, may be responsible for different oscillation patterns for neutrino and antineutrino and unconventional energy dependency of the oscillation phase or of the mixing angles. Future perspectives for possible CPT and Lorentz violating systems are also presented.
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16
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17
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Szczepańczyk MJ, Antelis JM, Benjamin M, Cavaglià M, Gondek-Rosińska D, Hansen T, Klimenko S, Morales MD, Moreno C, Mukherjee S, Nurbek G, Powell J, Singh N, Sitmukhambetov S, Szewczyk P, Valdez O, Vedovato G, Westhouse J, Zanolin M, Zheng Y. Detecting and reconstructing gravitational waves from the next galactic core-collapse supernova in the advanced detector era. Int J Clin Exp Med 2021. [DOI: 10.1103/physrevd.104.102002] [Citation(s) in RCA: 14] [Impact Index Per Article: 4.7] [Reference Citation Analysis] [Track Full Text] [Journal Information] [Subscribe] [Scholar Register] [Indexed: 11/07/2022]
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18
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Abstract
Neutrino leptonic flavor symmetry violation is the only evidence for physics beyond the standard model. Much of what we have learned on these particles is derived from the study of their natural sources, such as the Sun or core-collapse supernovae. Neutrino emission from supernovae is particularly interesting and leptonic flavor transformations in supernova neutrinos have attracted a lot of theoretical attention. Unfortunately, the emission of core-collapse supernovae is not fully understood: thus, an inescapable preliminary step to progress is to improve on that, and future neutrino observations can help. One pressing and answerable question concerns the time distribution of the supernova anti-neutrino events. We propose a class of models of the time distribution that describe emission curves similar to those theoretically expected and consistent with available observations from the data of supernova SN1987A. They have the advantages of being motivated on physical bases and easy to interpret; they are flexible and adaptable to the results of the observations from a future galactic supernova. Important general characteristics of these models are the presence of an initial ramp and that a significant portion of the signal is in the first second of the emission.
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19
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Abstract
The Virgo detector, based at the EGO (European Gravitational Observatory) and located in Cascina (Pisa), played a significant role in the development of the gravitational-wave astronomy. From its first scientific run in 2007, the Virgo detector has constantly been upgraded over the years; since 2017, with the Advanced Virgo project, the detector reached a high sensitivity that allowed the detection of several classes of sources and to investigate new physics. This work reports the main hardware upgrades of the detector and the main astrophysical results from the latest five years; future prospects for the Virgo detector are also presented.
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20
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Abstract
An overview of searches related to neutrinos of astronomical and astrophysical origin performed within the framework of the Standard-Model Extension is provided. For this effective field theory, key definitions, intriguing physical consequences, and the mathematical formalism are summarized within the neutrino sector to search for effects from a background that could lead to small deviations from Lorentz symmetry. After an introduction to the fundamental theory, examples of various experiments within the astronomical and astrophysical context are provided. Order-of-magnitude bounds of SME coefficients are shown illustratively for the tight constraints that this sector allows us to place on such violations.
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21
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de Gouvêa A, Martinez-Soler I, Perez-Gonzalez YF, Sen M. Fundamental physics with the diffuse supernova background neutrinos. Int J Clin Exp Med 2020. [DOI: 10.1103/physrevd.102.123012] [Citation(s) in RCA: 15] [Impact Index Per Article: 3.8] [Reference Citation Analysis] [Track Full Text] [Journal Information] [Subscribe] [Scholar Register] [Indexed: 11/07/2022]
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22
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Aharmim B, Ahmed S, Anthony A, Barros N, Beier E, Bellerive A, Beltran B, Bergevin M, Biller S, Blucher E, Bonventre R, Boudjemline K, Boulay M, Cai B, Callaghan E, Caravaca J, Chan Y, Chauhan D, Chen M, Cleveland B, Cox G, Dai X, Deng H, Descamps F, Detwiler J, Doe P, Doucas G, Drouin PL, Dunford M, Elliott S, Evans H, Ewan G, Farine J, Fergani H, Fleurot F, Ford R, Formaggio J, Gagnon N, Gilje K, Goon J, Graham K, Guillian E, Habib S, Hahn R, Hallin A, Hallman E, Harvey P, Hazama R, Heintzelman W, Heise J, Helmer R, Hime A, Howard C, Huang M, Jagam P, Jamieson B, Jelley N, Jerkins M, Keeter K, Klein J, Kormos L, Kos M, Kraus C, Krauss C, Krüger A, Kutter T, Kyba C, Labe K, Land B, Lange R, LaTorre A, Law J, Lawson I, Lesko K, Leslie J, Levine I, Loach J, MacLellan R, Majerus S, Mak H, Maneira J, Martin R, Mastbaum A, McCauley N, McDonald A, McGee S, Miller M, Monreal B, Monroe J, Nickel B, Noble A, O’Keeffe H, Oblath N, Okada C, Ollerhead R, Orebi Gann G, Oser S, Ott R, Peeters S, Poon A, Prior G, Reitzner S, Rielage K, Robertson B, Robertson R, Schwendener M, Secrest J, Seibert S, Simard O, Sinclair D, Skensved P, Sonley T, Stonehill L, Tešić G, Tolich N, Tsui T, Van Berg R, VanDevender B, Virtue C, Wall B, Waller D, Wan Chan Tseung H, Wark D, Wendland J, West N, Wilkerson J, Wilson J, Winchester T, Wright A, Yeh M, Zhang F, Zuber K. Search for
hep
solar neutrinos and the diffuse supernova neutrino background using all three phases of the Sudbury Neutrino Observatory. Int J Clin Exp Med 2020. [DOI: 10.1103/physrevd.102.062006] [Citation(s) in RCA: 6] [Impact Index Per Article: 1.5] [Reference Citation Analysis] [Track Full Text] [Journal Information] [Subscribe] [Scholar Register] [Indexed: 11/07/2022]
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23
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Acero M, Adamson P, Aliaga L, Alion T, Allakhverdian V, Anfimov N, Antoshkin A, Asquith L, Aurisano A, Back A, Backhouse C, Baird M, Balashov N, Baldi P, Bambah B, Bashar S, Bays K, Bending S, Bernstein R, Bhatnagar V, Bhuyan B, Bian J, Blair J, Booth A, Bour P, Bromberg C, Buchanan N, Butkevich A, Calvez S, Carroll T, Catano-Mur E, Childress S, Choudhary B, Coan T, Colo M, Corwin L, Cremonesi L, Davies G, Derwent P, Dharmapalan R, Ding P, Djurcic Z, Doyle D, Dukes E, Dung P, Duyang H, Edayath S, Ehrlich R, Feldman G, Filip P, Flanagan W, Frank M, Gallagher H, Gandrajula R, Gao F, Germani S, Giri A, Gomes R, Goodman M, Grichine V, Groh M, Group R, Guo B, Habig A, Hakl F, Hartnell J, Hatcher R, Heller K, Hewes J, Himmel A, Holin A, Huang J, Hylen J, Jediny F, Johnson C, Judah M, Kakorin I, Kalra D, Kaplan D, Keloth R, Klimov O, Koerner L, Kolupaeva L, Kotelnikov S, Kullenberg C, Kumar A, Kuruppu C, Kus V, Lackey T, Lang K, Li L, Lin S, Lokajicek M, Luchuk S, Magill S, Mann W, Marshak M, Martinez-Casales M, Matveev V, Mayes B, Méndez D, Messier M, Meyer H, Miao T, Miller W, Mishra S, Mislivec A, Mohanta R, Moren A, Mualem L, Muether M, Mufson S, Mulder K, Murphy R, Musser J, Naples D, Nayak N, Nelson J, Nichol R, Niner E, Norman A, Norrick A, Nosek T, Olshevskiy A, Olson T, Paley J, Patterson R, Pawloski G, Petrova O, Petti R, Plunkett R, Rafique A, Psihas F, Raj V, Rebel B, Rojas P, Ryabov V, Samoylov O, Sanchez M, Sánchez Falero S, Shanahan P, Sheshukov A, Singh P, Singh V, Smith E, Smolik J, Snopok P, Solomey N, Sousa A, Soustruznik K, Strait M, Suter L, Sutton A, Talaga R, Tapia Oregui B, Tas P, Thayyullathil R, Thomas J, Tiras E, Torbunov D, Tripathi J, Torun Y, Urheim J, Vahle P, Vasel J, Vokac P, Vrba T, Wallbank M, Warburton T, Wetstein M, Whittington D, Wojcicki S, Wolcott J, Yallappa Dombara A, Yonehara K, Yu S, Yu Y, Zadorozhnyy S, Zalesak J, Zhang Y, Zwaska R. Search for multimessenger signals in NOvA coincident with LIGO/Virgo detections. Int J Clin Exp Med 2020. [DOI: 10.1103/physrevd.101.112006] [Citation(s) in RCA: 4] [Impact Index Per Article: 1.0] [Reference Citation Analysis] [Track Full Text] [Journal Information] [Subscribe] [Scholar Register] [Indexed: 11/07/2022]
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24
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Fast-pairwise Collective Neutrino Oscillations Associated with Asymmetric Neutrino Emissions in Core-collapse Supernovae. ACTA ACUST UNITED AC 2019. [DOI: 10.3847/1538-4357/ab4cf2] [Citation(s) in RCA: 42] [Impact Index Per Article: 8.4] [Reference Citation Analysis] [Track Full Text] [Journal Information] [Subscribe] [Scholar Register] [Indexed: 11/18/2022]
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25
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Mendes RV. Commutative or noncommutative spacetime? Two length scales of noncommutativity. Int J Clin Exp Med 2019. [DOI: 10.1103/physrevd.99.123006] [Citation(s) in RCA: 2] [Impact Index Per Article: 0.4] [Reference Citation Analysis] [Track Full Text] [Journal Information] [Subscribe] [Scholar Register] [Indexed: 11/07/2022]
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26
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Low-latency Gravitational-wave Alerts for Multimessenger Astronomy during the Second Advanced LIGO and Virgo Observing Run. ACTA ACUST UNITED AC 2019. [DOI: 10.3847/1538-4357/ab0e8f] [Citation(s) in RCA: 62] [Impact Index Per Article: 12.4] [Reference Citation Analysis] [Track Full Text] [Journal Information] [Subscribe] [Scholar Register] [Indexed: 11/18/2022]
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27
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Kyutoku K, Kashiyama K. Detectability of thermal neutrinos from binary neutron-star mergers and implications for neutrino physics. Int J Clin Exp Med 2018. [DOI: 10.1103/physrevd.97.103001] [Citation(s) in RCA: 21] [Impact Index Per Article: 3.5] [Reference Citation Analysis] [Track Full Text] [Journal Information] [Subscribe] [Scholar Register] [Indexed: 11/07/2022]
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28
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Agafonova N, Fulgione W, Malgin A, Manukovskiy K, Ryazhskaya O, Yen S, Yudin A. Possible explanation of the neutrino signal from SN1987A detected with the LSD. EPJ WEB OF CONFERENCES 2018. [DOI: 10.1051/epjconf/201819103004] [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
On February 23 1987 in 2:52 UT the neutrino telescope LSD under Mont Blanc detected neutrino signal, which could not be explained within the framework of the standard collapse model. We show that the LSD signal could be a consequence of the detection of gamma-quanta emitted from neutron-capture reactions on by iron nuclei contained in the composition of the experimental setup. Neutrons are produced in neutrino-nuclei reactions in the surrounding granite rock and steel structures of the detector.
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29
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Wright WP, Kneller JP. Neutrino Intensity Interferometry: Measuring Protoneutron Star Radii During Core-Collapse Supernovae. PHYSICAL REVIEW LETTERS 2017; 119:051101. [PMID: 28949708 DOI: 10.1103/physrevlett.119.051101] [Citation(s) in RCA: 0] [Impact Index Per Article: 0] [Reference Citation Analysis] [Abstract] [Track Full Text] [Subscribe] [Scholar Register] [Received: 03/31/2017] [Indexed: 06/07/2023]
Abstract
Intensity interferometry is a technique that has been used to measure the size of sources ranging from the quark-gluon plasma formed in heavy ion collisions to the radii of stars. We investigate using the same technique to measure protoneutron star (PNS) radii with the neutrino signal received from a core-collapse supernovae. Using a full wave-packet analysis, including the neutrino mass for the first time, we derive criteria where the effect can be expected to provide the desired signal, and find that neutrinos from the next Galactic supernova should contain extractable PNS radius information.
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Affiliation(s)
- Warren P Wright
- Department of Physics, North Carolina State University, Raleigh, North Carolina 27695, USA
| | - James P Kneller
- Department of Physics, North Carolina State University, Raleigh, North Carolina 27695, USA
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30
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Nieto MM, Hayes AC, Wilson WB, Teeter CM, Stanbro WD. Detection of Antineutrinos for Nonproliferation. NUCL SCI ENG 2017. [DOI: 10.13182/nse05-a2493] [Citation(s) in RCA: 11] [Impact Index Per Article: 1.6] [Reference Citation Analysis] [Track Full Text] [Journal Information] [Subscribe] [Scholar Register] [Indexed: 11/12/2022]
Affiliation(s)
- Michael Martin Nieto
- Theoretical Division, Los Alamos National Laboratory Los Alamos, New Mexico 87545
| | - A. C. Hayes
- Theoretical Division, Los Alamos National Laboratory Los Alamos, New Mexico 87545
| | - William B. Wilson
- Theoretical Division, Los Alamos National Laboratory Los Alamos, New Mexico 87545
| | - Corinne M. Teeter
- Physics Division, Los Alamos National Laboratory Los Alamos, New Mexico 87545
| | - William D. Stanbro
- Nuclear Nonproliferation Division Los Alamos, Los Alamos National Laboratory Los Alamos, New Mexico 87545
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31
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Ibe M, Nakano W, Suzuki M. Constraints on
Lμ−Lτ
gauge interactions from rare kaon decay. Int J Clin Exp Med 2017. [DOI: 10.1103/physrevd.95.055022] [Citation(s) in RCA: 20] [Impact Index Per Article: 2.9] [Reference Citation Analysis] [Track Full Text] [Journal Information] [Subscribe] [Scholar Register] [Indexed: 11/07/2022]
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32
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NEUTRINO SIGNAL OF COLLAPSE-INDUCED THERMONUCLEAR SUPERNOVAE: THE CASE FOR PROMPT BLACK HOLE FORMATION IN SN 1987A. ACTA ACUST UNITED AC 2016. [DOI: 10.3847/0004-637x/828/1/31] [Citation(s) in RCA: 31] [Impact Index Per Article: 3.9] [Reference Citation Analysis] [Track Full Text] [Journal Information] [Subscribe] [Scholar Register] [Indexed: 11/18/2022]
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33
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A DARK ENERGY CAMERA SEARCH FOR MISSING SUPERGIANTS IN THE LMC AFTER THE ADVANCED LIGO GRAVITATIONAL-WAVE EVENT GW150914. ACTA ACUST UNITED AC 2016. [DOI: 10.3847/2041-8205/823/2/l34] [Citation(s) in RCA: 20] [Impact Index Per Article: 2.5] [Reference Citation Analysis] [Track Full Text] [Journal Information] [Subscribe] [Scholar Register] [Indexed: 11/18/2022]
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34
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Hayama K, Kuroda T, Kotake K, Takiwaki T. Coherent network analysis of gravitational waves from three-dimensional core-collapse supernova models. Int J Clin Exp Med 2015. [DOI: 10.1103/physrevd.92.122001] [Citation(s) in RCA: 29] [Impact Index Per Article: 3.2] [Reference Citation Analysis] [Track Full Text] [Journal Information] [Subscribe] [Scholar Register] [Indexed: 11/07/2022]
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35
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Izaguirre E, Krnjaic G, Schuster P, Toro N. Analyzing the Discovery Potential for Light Dark Matter. PHYSICAL REVIEW LETTERS 2015; 115:251301. [PMID: 26722912 DOI: 10.1103/physrevlett.115.251301] [Citation(s) in RCA: 10] [Impact Index Per Article: 1.1] [Reference Citation Analysis] [Abstract] [Track Full Text] [Subscribe] [Scholar Register] [Received: 05/12/2015] [Indexed: 06/05/2023]
Abstract
In this Letter, we determine the present status of sub-GeV thermal dark matter annihilating through standard model mixing, with special emphasis on interactions through the vector portal. Within representative simple models, we carry out a complete and precise calculation of the dark matter abundance and of all available constraints. We also introduce a concise framework for comparing different experimental approaches, and use this comparison to identify important ranges of dark matter mass and couplings to better explore in future experiments. The requirement that dark matter be a thermal relic sets a sharp sensitivity target for terrestrial experiments, and so we highlight complementary experimental approaches that can decisively reach this milestone sensitivity over the entire sub-GeV mass range.
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Affiliation(s)
- Eder Izaguirre
- Perimeter Institute for Theoretical Physics, Waterloo, ON N2L 2Y5, Canada
| | - Gordan Krnjaic
- Perimeter Institute for Theoretical Physics, Waterloo, ON N2L 2Y5, Canada
| | - Philip Schuster
- Perimeter Institute for Theoretical Physics, Waterloo, ON N2L 2Y5, Canada
| | - Natalia Toro
- Perimeter Institute for Theoretical Physics, Waterloo, ON N2L 2Y5, Canada
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36
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Adamson P, Anghel I, Ashby N, Aurisano A, Barr G, Bishai M, Blake A, Bock G, Bogert D, Bumgarner R, Cao S, Castromonte C, Childress S, Coelho J, Corwin L, Cronin-Hennessy D, de Jong J, Devan A, Devenish N, Diwan M, Escobar C, Evans J, Falk E, Feldman G, Fonville B, Frohne M, Gallagher H, Gomes R, Goodman M, Gouffon P, Graf N, Gran R, Grzelak K, Habig A, Hahn S, Hartnell J, Hatcher R, Hirschauer J, Holin A, Huang J, Hylen J, Irwin G, Isvan Z, James C, Jefferts S, Jensen D, Kafka T, Kasahara S, Koizumi G, Kordosky M, Kreymer A, Lang K, Ling J, Litchfield P, Lucas P, Mann W, Marshak M, Matsakis D, Mayer N, McKinley A, McGivern C, Medeiros M, Mehdiyev R, Meier J, Messier M, Miller W, Mishra S, Mitchell S, Moed Sher S, Moore C, Mualem L, Musser J, Naples D, Nelson J, Newman H, Nichol R, Nowak J, O’Connor J, Orchanian M, Pahlka R, Paley J, Parker T, Patterson R, Pawloski G, Perch A, Phan-Budd S, Plunkett R, Poonthottathil N, Powers E, Qiu X, Radovic A, Rebel B, Ridl K, Römisch S, Rosenfeld C, Rubin H, Sanchez M, Schneps J, Schreckenberger A, Schreiner P, Sharma R, Sousa A, Tagg N, Talaga R, Thomas J, Thomson M, Tian X, Timmons A, Tognini S, Toner R, Torretta D, Urheim J, Vahle P, Viren B, Weber A, Webb R, White C, Whitehead L, Whitehead L, Wojcicki S, Wright J, Zhang V, Zwaska R. Precision measurement of the speed of propagation of neutrinos using the MINOS detectors. Int J Clin Exp Med 2015. [DOI: 10.1103/physrevd.92.052005] [Citation(s) in RCA: 11] [Impact Index Per Article: 1.2] [Reference Citation Analysis] [Track Full Text] [Journal Information] [Subscribe] [Scholar Register] [Indexed: 11/07/2022]
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37
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Usman S, Jocher G, Dye S, McDonough W, Learned J. AGM2015: Antineutrino Global Map 2015. Sci Rep 2015; 5:13945. [PMID: 26323507 PMCID: PMC4555106 DOI: 10.1038/srep13945] [Citation(s) in RCA: 15] [Impact Index Per Article: 1.7] [Reference Citation Analysis] [Abstract] [Track Full Text] [Download PDF] [Figures] [Journal Information] [Subscribe] [Scholar Register] [Received: 01/12/2015] [Accepted: 08/11/2015] [Indexed: 11/13/2022] Open
Abstract
Every second greater than 10(25) antineutrinos radiate to space from Earth, shining like a faint antineutrino star. Underground antineutrino detectors have revealed the rapidly decaying fission products inside nuclear reactors, verified the long-lived radioactivity inside our planet, and informed sensitive experiments for probing fundamental physics. Mapping the anisotropic antineutrino flux and energy spectrum advance geoscience by defining the amount and distribution of radioactive power within Earth while critically evaluating competing compositional models of the planet. We present the Antineutrino Global Map 2015 (AGM2015), an experimentally informed model of Earth's surface antineutrino flux over the 0 to 11 MeV energy spectrum, along with an assessment of systematic errors. The open source AGM2015 provides fundamental predictions for experiments, assists in strategic detector placement to determine neutrino mass hierarchy, and aids in identifying undeclared nuclear reactors. We use cosmochemically and seismologically informed models of the radiogenic lithosphere/mantle combined with the estimated antineutrino flux, as measured by KamLAND and Borexino, to determine the Earth's total antineutrino luminosity at . We find a dominant flux of geo-neutrinos, predict sub-equal crust and mantle contributions, with ~1% of the total flux from man-made nuclear reactors.
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Affiliation(s)
- S.M. Usman
- Exploratory Science and Technology Branch, National Geospatial-Intelligence Agency, Springfield, VA, 22150, USA
| | | | - S.T. Dye
- Department of Physics and Astronomy, University of Hawaii, Honolulu, HI, 96822, USA
- Department of Natural Sciences, Hawaii Pacific University, Kaneohe, HI, 96744, USA
| | - W.F. McDonough
- Department of Geology, University of Maryland, College Park, MD, 20742, USA
| | - J.G. Learned
- Department of Physics and Astronomy, University of Hawaii, Honolulu, HI, 96822, USA
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38
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39
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Boggs SE, Harrison FA, Miyasaka H, Grefenstette BW, Zoglauer A, Fryer CL, Reynolds SP, Alexander DM, An H, Barret D, Christensen FE, Craig WW, Forster K, Giommi P, Hailey CJ, Hornstrup A, Kitaguchi T, Koglin JE, Madsen KK, Mao PH, Mori K, Perri M, Pivovaroff MJ, Puccetti S, Rana V, Stern D, Westergaard NJ, Zhang WW. 44
Ti gamma-ray emission lines from SN1987A reveal an asymmetric explosion. Science 2015; 348:670-1. [DOI: 10.1126/science.aaa2259] [Citation(s) in RCA: 85] [Impact Index Per Article: 9.4] [Reference Citation Analysis] [Track Full Text] [Journal Information] [Subscribe] [Scholar Register] [Indexed: 11/02/2022]
Affiliation(s)
- S. E. Boggs
- Space Sciences Laboratory, University of California, Berkeley, CA 94720, USA
| | - F. A. Harrison
- Cahill Center for Astronomy and Astrophysics, California Institute of Technology, Pasadena, CA 91125, USA
| | - H. Miyasaka
- Cahill Center for Astronomy and Astrophysics, California Institute of Technology, Pasadena, CA 91125, USA
| | - B. W. Grefenstette
- Cahill Center for Astronomy and Astrophysics, California Institute of Technology, Pasadena, CA 91125, USA
| | - A. Zoglauer
- Space Sciences Laboratory, University of California, Berkeley, CA 94720, USA
| | - C. L. Fryer
- CCS-2, Los Alamos National Laboratory, Los Alamos, NM 87545, USA
| | - S. P. Reynolds
- Physics Department, NC State University, Raleigh, NC 27695, USA
| | - D. M. Alexander
- Department of Physics, Durham University, Durham DH1 3LE, UK
| | - H. An
- Department of Physics, McGill University, Rutherford Physics Building, Montreal, Quebec H3A 2T8, Canada
| | - D. Barret
- Université de Toulouse, UPS-OMP, IRAP, Toulouse, France
- CNRS, Institut de Recherche en Astrophysique et Planétologie, 9 Av. colonel Roche, BP 44346, F-31028 Toulouse Cedex 4, France
| | - F. E. Christensen
- DTU Space, National Space Institute, Technical University of Denmark, Elektrovej 327, DK-2800 Lyngby, Denmark
| | - W. W. Craig
- Space Sciences Laboratory, University of California, Berkeley, CA 94720, USA
- Lawrence Livermore National Laboratory, Livermore, CA 94550, USA
| | - K. Forster
- Cahill Center for Astronomy and Astrophysics, California Institute of Technology, Pasadena, CA 91125, USA
| | - P. Giommi
- Agenzia Spaziale Italiana (ASI) Science Data Center, Via del Politecnico snc I-00133, Roma, Italy
| | - C. J. Hailey
- Columbia Astrophysics Laboratory, Columbia University, New York, NY 10027, USA
| | - A. Hornstrup
- DTU Space, National Space Institute, Technical University of Denmark, Elektrovej 327, DK-2800 Lyngby, Denmark
| | - T. Kitaguchi
- RIKEN Nishina Center, 2-1 Hirosawa, Wako, Saitama, 351-0198, Japan
| | - J. E. Koglin
- Kavli Institute for Particle Astrophysics and Cosmology, SLAC National Accelerator Laboratory, Menlo Park, CA 94025, USA
| | - K. K. Madsen
- Cahill Center for Astronomy and Astrophysics, California Institute of Technology, Pasadena, CA 91125, USA
| | - P. H. Mao
- Cahill Center for Astronomy and Astrophysics, California Institute of Technology, Pasadena, CA 91125, USA
| | - K. Mori
- Columbia Astrophysics Laboratory, Columbia University, New York, NY 10027, USA
| | - M. Perri
- Agenzia Spaziale Italiana (ASI) Science Data Center, Via del Politecnico snc I-00133, Roma, Italy
- INAF – Osservatorio Astronomico di Roma, via di Frascati 33, I-00040 Monteporzio, Italy
| | - M. J. Pivovaroff
- Lawrence Livermore National Laboratory, Livermore, CA 94550, USA
| | - S. Puccetti
- Agenzia Spaziale Italiana (ASI) Science Data Center, Via del Politecnico snc I-00133, Roma, Italy
- INAF – Osservatorio Astronomico di Roma, via di Frascati 33, I-00040 Monteporzio, Italy
| | - V. Rana
- Cahill Center for Astronomy and Astrophysics, California Institute of Technology, Pasadena, CA 91125, USA
| | - D. Stern
- Jet Propulsion Laboratory, California Institute of Technology, Pasadena, CA 91109, USA
| | - N. J. Westergaard
- DTU Space, National Space Institute, Technical University of Denmark, Elektrovej 327, DK-2800 Lyngby, Denmark
| | - W. W. Zhang
- NASA Goddard Space Flight Center, Greenbelt, MD 20771, USA
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40
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Chakraborty S, Bhattacharjee P, Kar K. Observing supernova neutrino light curve in future dark matter detectors. Int J Clin Exp Med 2014. [DOI: 10.1103/physrevd.89.013011] [Citation(s) in RCA: 25] [Impact Index Per Article: 2.5] [Reference Citation Analysis] [Track Full Text] [Journal Information] [Subscribe] [Scholar Register] [Indexed: 11/07/2022]
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41
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Bartos I, Beloborodov AM, Hurley K, Márka S. Detection prospects for GeV neutrinos from collisionally heated gamma-ray bursts with IceCube/DeepCore. PHYSICAL REVIEW LETTERS 2013; 110:241101. [PMID: 25165903 DOI: 10.1103/physrevlett.110.241101] [Citation(s) in RCA: 7] [Impact Index Per Article: 0.6] [Reference Citation Analysis] [Abstract] [Track Full Text] [Subscribe] [Scholar Register] [Received: 01/17/2013] [Revised: 04/23/2013] [Indexed: 06/03/2023]
Abstract
Jet reheating via nuclear collisions has recently been proposed as the main mechanism for gamma-ray burst (GRB) emission. In addition to producing the observed gamma rays, collisional heating must generate 10-100 GeV neutrinos, implying a close relation between the neutrino and gamma-ray luminosities. We exploit this theoretical relation to make predictions for possible GRB detections by IceCube + DeepCore. To estimate the expected neutrino signal, we use the largest sample of bursts observed by the Burst and Transient Source Experiment in 1991-2000. GRB neutrinos could have been detected if IceCube + DeepCore operated at that time. Detection of 10-100 GeV neutrinos would have significant implications, shedding light on the composition of GRB jets and their Lorentz factors. This could be an important target in designing future upgrades of the IceCube + DeepCore observatory.
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Affiliation(s)
- I Bartos
- Department of Physics, Columbia University, New York, New York 10027, USA and Columbia Astrophysics Laboratory, Columbia University, New York, New York 10027, USA
| | - A M Beloborodov
- Department of Physics, Columbia University, New York, New York 10027, USA and Columbia Astrophysics Laboratory, Columbia University, New York, New York 10027, USA
| | - K Hurley
- Space Sciences Laboratory, University of California, Berkeley, Berkeley, California 94720, USA
| | - S Márka
- Department of Physics, Columbia University, New York, New York 10027, USA and Columbia Astrophysics Laboratory, Columbia University, New York, New York 10027, USA
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42
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Pakvasa S, Joshipura A, Mohanty S. Explanation for the low flux of high-energy astrophysical muon neutrinos. PHYSICAL REVIEW LETTERS 2013; 110:171802. [PMID: 23679707 DOI: 10.1103/physrevlett.110.171802] [Citation(s) in RCA: 7] [Impact Index Per Article: 0.6] [Reference Citation Analysis] [Abstract] [Track Full Text] [Subscribe] [Scholar Register] [Received: 09/25/2012] [Revised: 12/04/2012] [Indexed: 06/02/2023]
Abstract
There has been some concern about the unexpected paucity of cosmic high-energy muon neutrinos in detectors probing the energy region beyond 1 PeV. As a possible solution we consider the possibility that some exotic neutrino property is responsible for reducing the muon neutrino flux at high energies from distant sources; specifically, we consider (i) neutrino decay and (ii) neutrinos being pseudo-Dirac-particles. This would provide a mechanism for the reduction of high-energy muon events in the IceCube detector, for example.
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Affiliation(s)
- Sandip Pakvasa
- Department of Physics and Astronomy, University of Hawaii, Honolulu, Hawaii 96822, USA
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43
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Bertolotti M. The Neutrino or, More Precisely, the Neutrinos: Elusive and Weird Particles, Able to Arrive from Very Far Away. CELESTIAL MESSENGERS 2013:229-252. [DOI: 10.1007/978-3-642-28371-0_11] [Citation(s) in RCA: 0] [Impact Index Per Article: 0] [Reference Citation Analysis] [Track Full Text] [Subscribe] [Scholar Register] [Indexed: 09/02/2023]
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44
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Agafonova NY, Aglietta M, Antonioli P, Ashikhmin VV, Bari G, Bertoni R, Bressan E, Bruno G, Dadykin VL, Fulgione W, Galeotti P, Garbini M, Ghia PL, Giusti P, Kemp E, Mal'gin AS, Miguez B, Molinario A, Persiani R, Pless IA, Ryasny VG, Ryazhskaya OG, Saavedra O, Sartorelli G, Shakyrianova IR, Selvi M, Trinchero GC, Vigorito C, Yakushev VF, Zichichi A, Razeto A. Measurement of the velocity of neutrinos from the CNGS beam with the large volume detector. PHYSICAL REVIEW LETTERS 2012; 109:070801. [PMID: 23006352 DOI: 10.1103/physrevlett.109.070801] [Citation(s) in RCA: 3] [Impact Index Per Article: 0.3] [Reference Citation Analysis] [Abstract] [Track Full Text] [Subscribe] [Scholar Register] [Received: 07/18/2012] [Indexed: 06/01/2023]
Abstract
We report the measurement of the time of flight of ∼17 GeV ν(μ) on the CNGS baseline (732 km) with the Large Volume Detector (LVD) at the Gran Sasso Laboratory. The CERN-SPS accelerator has been operated from May 10th to May 24th 2012, with a tightly bunched-beam structure to allow the velocity of neutrinos to be accurately measured on an event-by-event basis. LVD has detected 48 neutrino events, associated with the beam, with a high absolute time accuracy. These events allow us to establish the following limit on the difference between the neutrino speed and the light velocity: -3.8 × 10(-6) < (v(ν)-c)/c < 3.1 × 10(-6) (at 99% C.L.). This value is an order of magnitude lower than previous direct measurements.
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Affiliation(s)
- N Yu Agafonova
- Institute for Nuclear Research, Russian Academy of Sciences, Moscow, Russia
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45
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46
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Bezrukov F, Lee HM. Model dependence of the bremsstrahlung effects from the superluminal neutrino at OPERA. Int J Clin Exp Med 2012. [DOI: 10.1103/physrevd.85.031901] [Citation(s) in RCA: 15] [Impact Index Per Article: 1.3] [Reference Citation Analysis] [Track Full Text] [Journal Information] [Subscribe] [Scholar Register] [Indexed: 11/07/2022]
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47
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Cowsik R, Nussinov S, Sarkar U. Superluminal neutrinos at OPERA confront pion decay kinematics. PHYSICAL REVIEW LETTERS 2011; 107:251801. [PMID: 22243066 DOI: 10.1103/physrevlett.107.251801] [Citation(s) in RCA: 6] [Impact Index Per Article: 0.5] [Reference Citation Analysis] [Abstract] [Track Full Text] [Subscribe] [Scholar Register] [Received: 10/02/2011] [Revised: 12/05/2011] [Indexed: 05/31/2023]
Abstract
Violation of Lorentz invariance (VLI) has been suggested as an explanation of the superluminal velocities of muon neutrinos reported by OPERA. In this Letter, we show that the amount of VLI required to explain this result poses severe difficulties with the kinematics of the pion decay, extending its lifetime and reducing the momentum carried away by the neutrinos. We show that the OPERA experiment limits α=(ν(ν)-c)/c<4×10(-6). We then take recourse to cosmic-ray data on the spectrum of muons and neutrinos generated in Earth's atmosphere to provide a stronger bound on VLI: (ν-c)/c<10(-12).
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Affiliation(s)
- Ramanath Cowsik
- Department of Physics and McDonnell Center for the Space Sciences, Washington University, St. Louis, Missouri 63130, USA
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48
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Bi XJ, Yin PF, Yu ZH, Yuan Q. Constraints and tests of the OPERA superluminal neutrinos. PHYSICAL REVIEW LETTERS 2011; 107:241802. [PMID: 22242991 DOI: 10.1103/physrevlett.107.241802] [Citation(s) in RCA: 9] [Impact Index Per Article: 0.7] [Reference Citation Analysis] [Abstract] [Track Full Text] [Subscribe] [Scholar Register] [Received: 10/13/2011] [Indexed: 05/31/2023]
Abstract
The superluminal neutrinos detected by OPERA indicate Lorentz invariance violation (LIV) of the neutrino sector at the order of 10(-5). We study the implications of the result in this work. We find that such a large LIV implied by OPERA data will make the neutrino production process π → μ + ν(μ) kinematically forbidden for a neutrino energy greater than about 5 GeV. The OPERA detection of neutrinos at 40 GeV can constrain the LIV parameter to be smaller than 3×10(-7). Furthermore, the neutrino decay in the LIV framework will modify the neutrino spectrum greatly. The atmospheric neutrino spectrum measured by the IceCube Collaboration can constrain the LIV parameter to the level of 10(-12). The future detection of astrophysical neutrinos of galactic sources is expected to be able to give an even stronger constraint on the LIV parameter of neutrinos.
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Affiliation(s)
- Xiao-Jun Bi
- Key Laboratory of Particle Astrophysics, Institute of High Energy Physics, Chinese Academy of Sciences, Beijing 100049, China
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49
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Cohen AG, Glashow SL. Pair creation constrains superluminal neutrino propagation. PHYSICAL REVIEW LETTERS 2011; 107:181803. [PMID: 22107624 DOI: 10.1103/physrevlett.107.181803] [Citation(s) in RCA: 17] [Impact Index Per Article: 1.3] [Reference Citation Analysis] [Abstract] [Track Full Text] [Subscribe] [Scholar Register] [Received: 10/04/2011] [Indexed: 05/31/2023]
Abstract
The OPERA collaboration claims that muon neutrinos with a mean energy of 17.5 GeV travel 730 km from CERN to the Gran Sasso at a speed exceeding that of light by about 7.5 km/s or 25 ppm. However, we show that superluminal neutrinos may lose energy rapidly via the bremsstrahlung of electron-positron pairs (ν → ν + e- + e+). For the claimed superluminal velocity and at the stated mean energy, we find that most of the neutrinos would have suffered several pair emissions en route, causing the beam to be depleted of higher energy neutrinos. This presents a significant challenge to the superluminal interpretation of the OPERA data. Furthermore, we appeal to Super-Kamiokande and IceCube data to establish strong new limits on the superluminal propagation of high-energy neutrinos.
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Affiliation(s)
- Andrew G Cohen
- Physics Department, Boston University, Boston, Massachusetts 02215, USA.
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50
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Matsuura M, Dwek E, Meixner M, Otsuka M, Babler B, Barlow MJ, Roman-Duval J, Engelbracht C, Sandstrom K, Lakićević M, van Loon JT, Sonneborn G, Clayton GC, Long KS, Lundqvist P, Nozawa T, Gordon KD, Hony S, Panuzzo P, Okumura K, Misselt KA, Montiel E, Sauvage M. Herschel Detects a Massive Dust Reservoir in Supernova 1987A. Science 2011; 333:1258-61. [PMID: 21737700 DOI: 10.1126/science.1205983] [Citation(s) in RCA: 252] [Impact Index Per Article: 19.4] [Reference Citation Analysis] [Track Full Text] [Journal Information] [Subscribe] [Scholar Register] [Indexed: 11/02/2022]
Affiliation(s)
- M. Matsuura
- Astrophysics Group, Department of Physics and Astronomy, University College London, Gower Street, London WC1E 6BT, UK
- Mullard Space Science Laboratory, University College London, Holmbury St. Mary, Dorking, Surrey RH5 6NT, UK
| | - E. Dwek
- Observational Cosmology Laboratory, Code 665, NASA Goddard Space Flight Center, Greenbelt, MD 20771, USA
| | - M. Meixner
- Space Telescope Science Institute, 3700 San Martin Drive, Baltimore, MD 21218, USA
| | - M. Otsuka
- Space Telescope Science Institute, 3700 San Martin Drive, Baltimore, MD 21218, USA
| | - B. Babler
- Department of Astronomy, 475 North Charter St., University of Wisconsin, Madison, WI 53706, USA
| | - M. J. Barlow
- Astrophysics Group, Department of Physics and Astronomy, University College London, Gower Street, London WC1E 6BT, UK
| | - J. Roman-Duval
- Space Telescope Science Institute, 3700 San Martin Drive, Baltimore, MD 21218, USA
| | - C. Engelbracht
- Steward Observatory, University of Arizona, Tucson, AZ 85721, USA
| | - K. Sandstrom
- Max-Planck-Institut für Astronomie, Königstuhl 17, D-69117 Heidelberg, Germany
| | - M. Lakićević
- Astrophysics Group, Lennard-Jones Laboratories, Keele University, ST5 5BG, UK
- European Southern Observatory, Karl Schwarschild Straße 2, D-85748 Garching bei München, Germany
| | - J. Th. van Loon
- Astrophysics Group, Lennard-Jones Laboratories, Keele University, ST5 5BG, UK
| | - G. Sonneborn
- Observational Cosmology Laboratory, Code 665, NASA Goddard Space Flight Center, Greenbelt, MD 20771, USA
| | - G. C. Clayton
- Louisiana State University, Department of Physics and Astronomy, 233-A Nicholson Hall, Tower Drive, Baton Rouge, LA 70803–4001, USA
| | - K. S. Long
- Space Telescope Science Institute, 3700 San Martin Drive, Baltimore, MD 21218, USA
| | - P. Lundqvist
- Department of Astronomy, The Oskar Klein Centre, AlbaNova University Center, Stockholm University, SE-106 91 Stockholm, Sweden
| | - T. Nozawa
- Institute for the Physics and Mathematics of the Universe, University of Tokyo, Kashiwa, Chiba 277-8583, Japan
| | - K. D. Gordon
- Space Telescope Science Institute, 3700 San Martin Drive, Baltimore, MD 21218, USA
| | - S. Hony
- Commissariat à l’Energie Atomique et aux Energies Alternatives, Laboratoire Astrophysique, Instrumentation et Modélisation, Irfu/SAp, Orme des Merisiers, F-91191 Gif-sur-Yvette, France
| | - P. Panuzzo
- Commissariat à l’Energie Atomique et aux Energies Alternatives, Laboratoire Astrophysique, Instrumentation et Modélisation, Irfu/SAp, Orme des Merisiers, F-91191 Gif-sur-Yvette, France
| | - K. Okumura
- Commissariat à l’Energie Atomique et aux Energies Alternatives, Laboratoire Astrophysique, Instrumentation et Modélisation, Irfu/SAp, Orme des Merisiers, F-91191 Gif-sur-Yvette, France
| | - K. A. Misselt
- Steward Observatory, University of Arizona, Tucson, AZ 85721, USA
| | - E. Montiel
- Steward Observatory, University of Arizona, Tucson, AZ 85721, USA
| | - M. Sauvage
- Commissariat à l’Energie Atomique et aux Energies Alternatives, Laboratoire Astrophysique, Instrumentation et Modélisation, Irfu/SAp, Orme des Merisiers, F-91191 Gif-sur-Yvette, France
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