Proton acceleration in thermonuclear nova explosions revealed by gamma   rays

MAGIC Collaboration: V. A. Acciari (1); S. Ansoldi (2,42); L. A.; Antonelli (3); A. Arbet Engels (4); M. Artero (5); K. Asano (6); D. Baack; (7); A. Babi\'c (8); A. Baquero (9); U. Barres de Almeida (10); J. A. Barrio; (9); I. Batkovi\'c (11); J. Becerra Gonz\'alez (1); W. Bednarek (12); L.; Bellizzi (13); E. Bernardini (14); M. Bernardos (11); A. Berti (15); J.; Besenrieder (15); W. Bhattacharyya (14); C. Bigongiari (3); A. Biland (4); O.; Blanch (5); H. B\"okenkamp (7); G. Bonnoli (16); \v{Z}. Bo\v{s}njak (8); G.; Busetto (11); R. Carosi (17); G. Ceribella (15); M. Cerruti (18); Y. Chai; (15); A. Chilingarian (19); S. Cikota (8); S. M. Colak (5); E. Colombo (1),; J. L. Contreras (9); J. Cortina (20); S. Covino (3); G. D'Amico (15,43); V.; D'Elia (3); P. Da Vela (17,44); F. Dazzi (3); A. De Angelis (11); B. De Lotto; (2); A. Del Popolo (21); M. Delfino (5,45); J. Delgado (5,45); C. Delgado; Mendez (20); D. Depaoli (22); F. Di Pierro (22); L. Di Venere (23); E. Do; Souto Espi\~neira (5); D. Dominis Prester (24); A. Donini (2); D. Dorner; (25); M. Doro (11); D. Elsaesser (7); V. Fallah Ramazani (26,46); L. Fari\~na; Alonso (5); A. Fattorini (7); M. V. Fonseca (9); L. Font (27); C. Fruck (15),; S. Fukami (4); Y. Fukazawa (28); R. J. Garc\'ia L\'opez (1); M. Garczarczyk; (14); S. Gasparyan (29); M. Gaug (27); N. Giglietto (23); F. Giordano (23),; P. Gliwny (12); N. Godinovi\'c (30); J. G. Green (15); D. Green (15); D.; Hadasch (6); A. Hahn (15); T. Hassan (20); L. Heckmann (15); J. Herrera (1),; J. Hoang (9,47); D. Hrupec (31); M. H\"utten (6); T. Inada (6); K. Ishio; (12); Y. Iwamura (6); I. Jim\'enez Mart\'inez (20); J. Jormanainen (26); L.; Jouvin (5); D. Kerszberg (5); Y. Kobayashi (6); H. Kubo (32); J. Kushida; (33); A. Lamastra (3); D. Lelas (30); F. Leone (3); E. Lindfors (26); L.; Linhoff (7); S. Lombardi (3); F. Longo (2,48); R. L\'opez-Coto (11); M.; L\'opez-Moya (9); A. L\'opez-Oramas (1); S. Loporchio (23); B. Machado de; Oliveira Fraga (10); C. Maggio (27); P. Majumdar (34); M. Makariev (35); M.; Mallamaci (11); G. Maneva (35); M. Manganaro (24); K. Mannheim (25); L.; Maraschi (3); M. Mariotti (11); M. Mart\'inez (5); A. Mas Aguilar (9); D.; Mazin (6,49); S. Menchiari (13); S. Mender (7); S. Mi\'canovi\'c (24); D.; Miceli (2,50); T. Miener (9); J. M. Miranda (13); R. Mirzoyan (15); E. Molina; (18); A. Moralejo (5); D. Morcuende (9); V. Moreno (27); E. Moretti (5); T.; Nakamori (36); L. Nava (3); V. Neustroev (37); M. Nievas Rosillo (1); C.; Nigro (5); K. Nilsson (26); K. Nishijima (33); K. Noda (6); S. Nozaki (32),; Y. Ohtani (6); T. Oka (32); J. Otero-Santos (1); S. Paiano (3); M. Palatiello; (2); D. Paneque (15); R. Paoletti (13); J. M. Paredes (18); L. Pavleti\'c; (24); P. Pe\~nil (9); M. Persic (2,51); M. Pihet (15); P. G. Prada Moroni; (17); E. Prandini (11); C. Priyadarshi (5); I. Puljak (30); W. Rhode (7); M.; Rib\'o (18); J. Rico (5); C. Righi (3); A. Rugliancich (17); N. Sahakyan; (29); T. Saito (6); S. Sakurai (6); K. Satalecka (14); F. G. Saturni (3); B.; Schleicher (25); K. Schmidt (7); T. Schweizer (15); J. Sitarek (6); I.; \v{S}nidari\'c (38); D. Sobczynska (12); A. Spolon (11); A. Stamerra (3); J.; Stri\v{s}kovi\'c (31); D. Strom (15); M. Strzys (6); Y. Suda (28); T. Suri\'c; (38); M. Takahashi (6); R. Takeishi (6); F. Tavecchio (3); P. Temnikov (35),; T. Terzi\'c (24); M. Teshima (15,52); L. Tosti (39); S. Truzzi (13); A.; Tutone (3); S. Ubach (27); J. van Scherpenberg (15); G. Vanzo (1); M. Vazquez; Acosta (1); S. Ventura (13); V. Verguilov (35); C. F. Vigorito (22); V.; Vitale (40); I. Vovk (6); M. Will (15); C. Wunderlich (13); T. Yamamoto (41),; D. Zari\'c (30); F. Ambrosino (53); M. Cecconi (54); G. Catanzaro (55); C.; Ferrara (55); A. Frasca (55); M. Munari (55); L. Giustolisi (55); J.; Alonso-Santiago (55); M. Giarrusso (56); U. Munari (57); P. Valisa (58) ((1); Instituto de Astrofisica de Canarias; La Laguna (Tenerife); Spain; (2); Universit\`a di Udine; INFN Trieste; Italy; Udine; Italy; (3) INAF -; National Institute for Astrophysics; Roma; Italy; (4) ETH Z\"urich; Institute; for Particle Physics; Z\"urich; Switzerland; (5) Institut de F\'isica d'Altes; Energies (IFAE); The Barcelona Institute of Science; Technology (BIST),; E-08193 Bellaterra (Barcelona); Spain; Bellaterra (Barcelona); Spain; (6); Japanese MAGIC Group: ICRR; The University of Tokyo; Chiba; Japan; (7); Technische Universit\"at Dortmund; Dortmund; Germany; (8) Croatian MAGIC; Group: University of Zagreb; Faculty of Electrical Engineering; Computing; (FER); Zagreb; Croatia; (9) IPARCOS Institute; EMFTEL Department,; Universidad Complutense de Madrid; Madrid; Spain; (10) Centro Brasileiro de; Pesquisas F\'isicas (CBPF); Rio de Janeiro; Brazil; (11) Dipartimento di; Fisica e Astronomia dell'Universit\`a; Sezione INFN; Padova; Italy,; Padova; Italy; (12) University of Lodz; Faculty of Physics; Applied; Informatics; Department of Astrophysics; Lodz; Poland; Lodz; Poland; (13); Dipartimento SFTA; Sezione di Fisica; Universit\`a di Siena; INFN sez. di; Pisa; Siena; Italy; (14) Deutsches Elektronen-Synchrotron (DESY) Zeuthen,; Zeuthen; Germany; (15) Max-Planck-Institut f\"ur Physik; M\"unchen,; M\"unchen; Germany; (16) Instituto de Astrof\'isica de Andaluc\'ia - CSIC,; Granada; Spain; (17) Universita di Pisa; INFN Pisa; Pisa; Italy; (18); Universitat de Barcelona; Barcelona; Spain; (19) Armenian MAGIC Group: A.; Alikhanyan National Science Laboratory; Yerevan; Armenia; (20) Centro de; Investigaciones Energeticas; Medioambientales y Tecnologicas; Madrid; Spain,; (21) INFN MAGIC Group: INFN Sezione di Catania; Catania; Italy; (22) INFN; MAGIC Group: INFN Sezione di Torino; Universit\`a degli Studi di Torino,; Torino; Italy; (23) INFN MAGIC Group: INFN Sezione di Bari; Dipartimento; Interateneo di Fisica dell'Universit\`a e del Politecnico di Bari; Bari,; Italy; (24) Croatian MAGIC Group: University of Rijeka; Department of; Physics; Rijeka; Croatia; (25) Institut f\"ur Theoretische Physik und; Astrophysik; Fakult\"at f\"ur Physik und Astronomie; Universit\"at; W\"urzburg; W\"urzburg; Germany; (26) Finnish MAGIC Group: Finnish Centre for; Astronomy with ESO; University of Turku; Turku; Finland; (27) Universitat; Aut\`onoma de Barcelona; Barcelona; Spain; (28) Japanese MAGIC Group: Physics; Program; Graduate School of Advanced Science; Engineering; Hiroshima; University; Hiroshima; Japan; (29) Armenian MAGIC Group: ICRANet-Armenia at; NAS RA; Yerevan; Armenia; (30) Croatian MAGIC Group: University of Split,; Faculty of Electrical Engineering; Mechanical Engineering; Naval; Architecture (FESB); Split; Croatia; (31) Croatian MAGIC Group: Josip Juraj; Strossmayer University of Osijek; Department of Physics; Osijek; Croatia,; (32) Japanese MAGIC Group: Department of Physics; Kyoto University; Kyoto,; Japan; (33) Japanese MAGIC Group: Department of Physics; Tokai University,; Kanagawa; Japan; (34) Saha Institute of Nuclear Physics; HBNI; Kolkata,; India; (35) Institute for Nuclear Research; Nuclear Energy; Sofia,; Bulgaria; (36) Japanese MAGIC Group: Department of Physics; Yamagata; University; Yamagata; Japan; (37) Finnish MAGIC Group: Astronomy Research; Unit; University of Oulu; Oulu; Finland; (38) Croatian MAGIC Group: Ruder; Boskovic Institute; Zagreb; Croatia; (39) INFN MAGIC Group: INFN Sezione di; Perugia; Perugia; Italy; (40) INFN MAGIC Group: INFN Roma Tor Vergata; Roma,; Italy; (41) Japanese MAGIC Group: Department of Physics; Konan University,; Kobe; Japan; (42) also at International Center for Relativistic Astrophysics; (ICRA); Rome; Italy; (43) now at Department for Physics; Technology,; University of Bergen; NO-5020; Norway; (44) now at University of Innsbruck,; (45) also at Port d'Informaci\'o Cient\'ifica (PIC); E-08193 Bellaterra; (Barcelona); Spain; (46) now at Ruhr-Universit\"at Bochum; Fakult\"at f\"ur; Physik und Astronomie; Astronomisches Institut (AIRUB); 44801 Bochum,; Germany; (47) now at Department of Astronomy; University of California; Berkeley; Berkeley CA; (48) also at Dipartimento di Fisica; Universit\`a di; Trieste; I-34127 Trieste; Italy; (49) Max-Planck-Institut f\"ur Physik,; M\"unchen; Germany; (50) now at Laboratoire d'Annecy de Physique des; Particules (LAPP); CNRS-IN2P3; 74941 Annecy Cedex; France; (51) also at INAF; Trieste; Dept. of Physics; Astronomy; University of Bologna; Bologna,; Italy; (52) Japanese MAGIC Group: Institute for Cosmic Ray Research (ICRR),; The University of Tokyo; Kashiwa; 277-8582 Chiba; Japan; (53) INAF -; Osservatorio Astrofisico di Roma; Monteporzio Catone (Roma) Italy; (54) INAF; - Fund. Galileo Galilei; Bren\~a Baja (La Palma); Canary Islands; Spain; (55); INAF - Osservatorio Astrofisico di Catania; Via S. Sofia 78; 95123 Catania,; Italy; (56) INFN - Laboratori Nazionali del Sud; Catania; Italy; (57) INAF -; Osservatorio Astronomico di Padova; I-36012 Asiago (Vi); Italy; (58) ANS; Collaboration; c/o Astronomical Observatory; Asiago (VI); Italy)

arXiv:2202.07681·astro-ph.HE·November 11, 2022·1 cites

Proton acceleration in thermonuclear nova explosions revealed by gamma rays

MAGIC Collaboration: V. A. Acciari (1), S. Ansoldi (2,42), L. A., Antonelli (3), A. Arbet Engels (4), M. Artero (5), K. Asano (6), D. Baack, (7), A. Babi\'c (8), A. Baquero (9), U. Barres de Almeida (10), J. A. Barrio, (9), I. Batkovi\'c (11), J. Becerra Gonz\'alez (1)

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TL;DR

This paper reports the first detection of gamma rays from a nova in the 60-250 GeV range, revealing that protons are accelerated to hundreds of GeV during nova explosions, which could influence cosmic ray populations.

Contribution

It provides the first detailed characterization of gamma-ray emission in the 60-250 GeV range from a nova, demonstrating proton acceleration to hundreds of GeV in such events.

Findings

01

Gamma rays detected from RS Ophiuchi nova in 60-250 GeV range.

02

Protons are accelerated to hundreds of GeV in nova shocks.

03

Potential formation of cosmic ray bubbles around recurrent novae.

Abstract

Classical novae are cataclysmic binary star systems in which the matter of a companion star is accreted on a white dwarf (WD). Accumulation of hydrogen in a layer eventually causes a thermonuclear explosion on the surface of the WD, brightening the WD to ~10^5 solar luminosities and triggering ejection of the accumulated matter.They provide extreme conditions required to accelerate particles, electrons or protons, to high energies. Here we present the detection of gamma rays by the MAGIC telescopes from the 2021 outburst of RS Ophiuchi (RS Oph), a recurrent nova with a red giant (RG) companion, that allowed us, for the first time, to accurately characterize the emission from a nova in the 60 GeV to 250 GeV energy range. The theoretical interpretation of the combined Fermi-LAT and MAGIC data suggests that protons are accelerated to hundreds of GeV in the nova shock. Such protons should…

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Taxonomy

TopicsAstrophysical Phenomena and Observations · Gamma-ray bursts and supernovae · Pulsars and Gravitational Waves Research