High-energy emission from a magnetar giant flare in the Sculptor galaxy

被引：25

作者：

Ajello, M. ^{[1
]}

Atwood, W. B. ^{[2
,3
]}

Axelsson, M. ^{[4
,5
]}

Baldini, L. ^{[6
,7
]}

Barbiellini, G. ^{[8
,9
]}

Baring, M. G. ^{[10
]}

Bastieri, D. ^{[11
,12
]}

Bellazzini, R. ^{[7
]}

Berretta, A. ^{[13
]}

Bissaldi, E. ^{[14
,15
,16
]}

Blandford, R. D. ^{[17
,18
]}

Bonino, R. ^{[19
,20
]}

Bregeon, J. ^{[21
]}

Bruel, P. ^{[22
]}

Buehler, R. ^{[23
]}

Burns, E. ^{[24
,25
]}

Buson, S. ^{[26
]}

Cameron, R. A. ^{[17
,18
]}

Caraveo, P. A. ^{[27
]}

Cavazzuti, E. ^{[28
]}

Chen, S. ^{[11
,29
]}

Cheung, C. C. ^{[30
]}

Chiaro, G. ^{[27
]}

Ciprini, S. ^{[31
,32
]}

Costantin, D. ^{[33
]}

Crnogorcevic, M. ^{[34
]}

Cutini, S. ^{[35
]}

D'Ammando, F. ^{[36
]}

de la Torre Luque, P. ^{[14
,15
]}

de Palma, F. ^{[19
]}

Digel, S. W. ^{[17
,18
]}

Di Lalla, N. ^{[17
,18
]}

Di Venere, L. ^{[14
,15
,16
]}

Dirirsa, F. Fana ^{[37
]}

Fukazawa, Y. ^{[38
]}

Funk, S. ^{[39
]}

Fusco, P. ^{[14
,15
,16
]}

Gargano, F. ^{[16
]}

Giglietto, N. ^{[14
,15
,16
]}

Gill, R. ^{[40
,41
]}

Giordano, F. ^{[14
,15
,16
]}

Giroletti, M. ^{[36
]}

Granot, J. ^{[41
]}

Green, D. ^{[42
]}

Grenier, I. A. ^{[43
]}

Griffin, S. ^{[25
]}

Guiriec, S. ^{[25
,40
]}

Hays, E. ^{[25
]}

Horan, D. ^{[22
]}

Johannesson, G. ^{[44
,45
,46
]}

机构：

[1] Clemson Univ, Dept Phys & Astron, Kinard Lab Phys, Clemson, SC 29634 USA

[2] Univ Calif Santa Cruz, Santa Cruz Inst Particle Phys, Dept Phys, Santa Cruz, CA 95064 USA

[3] Univ Calif Santa Cruz, Dept Astron & Astrophys, Santa Cruz, CA 95064 USA

[4] Stockholm Univ, Dept Phys, Stockholm, Sweden

[5] KTH Royal Inst Technol, Dept Phys, Stockholm, Sweden

[6] Univ Pisa, Pisa, Italy

[7] Ist Nazl Fis Nucl, Pisa, Italy

[8] Ist Nazl Fis Nucl, Trieste, Italy

[9] Univ Trieste, Dipartimento Fis, Trieste, Italy

[10] Rice Univ, Dept Phys & Astron, Houston, TX USA

[11] Ist Nazl Fis Nucl, Padua, Italy

[12] Univ Padua, Dipartimento Fis & Astron Galileo Galilei, Padua, Italy

[13] Univ Perugia, Dipartimento Fis, Perugia, Italy

[14] M Merlin Univ, Dipartimento Fis, Bari, Italy

[15] Politecn Bari, Bari, Italy

[16] Ist Nazl Fis Nucl, Bari, Italy

[17] Stanford Univ, Dept Phys, WW Hansen Expt Phys Lab, Kavli Inst Particle Astrophys & Cosmol, Stanford, CA 94305 USA

[18] Stanford Univ, SLAC Natl Accelerator Lab, Stanford, CA 94305 USA

[19] Ist Nazl Fis Nucl, Turin, Italy

[20] Univ Torino, Dipartimento Fis, Turin, Italy

[21] Univ Montpellier, Lab Universe & Particules Montpellier, CNRS, IN2P3, Montpellier, France

[22] Ecole Polytechn, Lab Leprince Ringuet, CNRS, IN2P3, Palaiseau, France

[23] Deutsches Elektronen Synchrotron DESY, Zeuthen, Germany

[24] Louisiana State Univ, Dept Phys & Astron, Baton Rouge, LA 70803 USA

[25] NASA, Goddard Space Flight Ctr, Greenbelt, MD USA

[26] Univ Wurzburg, Inst Theoret Phys & Astrophys, Wurzburg, Germany

[27] INAF Ist Astrofis Spaziale & Fis Cosm Milano, Milan, Italy

[28] Italian Space Agcy, Rome, Italy

[29] Univ Padua, Dept Phys & Astron, Padua, Italy

[30] Naval Res Lab, Space Sci Div, Washington, DC 20375 USA

[31] Ist Nazl Fis Nucl, Rome, Italy

[32] Agenzia Spaziale Italiana, Space Sci Data Ctr, Rome, Italy

[33] Univ Padua, Dept Stat Sci, Padua, Italy

[34] Univ Maryland, Dept Astron, College Pk, MD 20742 USA

[35] Ist Nazl Fis Nucl, Perugia, Italy

[36] INAF Ist Radioastron, Bologna, Italy

[37] Univ Johannesburg, Dept Phys, Johannesburg, South Africa

[38] Hiroshima Univ, Dept Phys Sci, Hiroshima, Japan

[39] Friedrich Alexander Univ Erlangen Nurnberg, Erlangen Ctr Astroparticle Phys, Erlangen, Germany

[40] George Washington Univ, Dept Phys, Washington, DC 20052 USA

[41] Open Univ Israel, Dept Nat Sci, Raanana, Israel

[42] Max Planck Inst Phys & Astrophys, Munich, Germany

[43] Univ Paris Diderot, Univ Paris Saclay, CNRS, AIM,CEA, Gif Sur Yvette, France

[44] Univ Iceland, Sci Inst, Reykjavik, Iceland

[45] Royal Inst Technol, Nordita, Stockholm, Sweden

[46] Stockholm Univ, Stockholm, Sweden

[47] Oskar Klein Ctr Cosmoparticle Phys, Stockholm, Sweden

[48] Dalarna Univ, Sch Educ Hlth & Social Studies, Nat Sci, Falun, Sweden

[49] Leopold Franzens Univ Innsbruck, Inst Astro & Teilchenphys, Innsbruck, Austria

[50] Hiroshima Univ, Hiroshima Astrophys Sci Ctr, Hiroshima, Japan

来源：

NATURE ASTRONOMY | 2021年 / 5卷 / 04期

关键词：

SOFT-GAMMA-REPEATER; RADIO-SOURCES; NEBULA; SGR-1806-20; MECHANISM;

D O I：

10.1038/s41550-020-01287-8

中图分类号：

P1 [天文学];

学科分类号：

0704 ;

摘要：

Magnetars are the most highly magnetized neutron stars in the cosmos (with magnetic field 10(13)-10(15) G). Giant flares from magnetars are rare, short-duration (about 0.1 s) bursts of hard X-rays and soft gamma rays(1,2). Owing to the limited sensitivity and energy coverage of previous telescopes, no magnetar giant flare has been detected at gigaelectronvolt (GeV) energies. Here, we report the discovery of GeV emission from a magnetar giant flare on 15 April 2020 (refs. (3,4) and A. J. Castro-Tirado et al., manuscript in preparation). The Large Area Telescope (LAT) on board the Fermi Gamma-ray Space Telescope detected GeV gamma rays from 19 s until 284 s after the initial detection of a signal in the megaelectronvolt (MeV) band. Our analysis shows that these gamma rays are spatially associated with the nearby (3.5 megaparsecs) Sculptor galaxy and are unlikely to originate from a cosmological gamma-ray burst. Thus, we infer that the gamma rays originated with the magnetar giant flare in Sculptor. We suggest that the GeV signal is generated by an ultra-relativistic outflow that first radiates the prompt MeV-band photons, and then deposits its energy far from the stellar magnetosphere. After a propagation delay, the outflow interacts with environmental gas and produces shock waves that accelerate electrons to very high energies; these electrons then emit GeV gamma rays as optically thin synchrotron radiation. This observation implies that a relativistic outflow is associated with the magnetar giant flare, and suggests the possibility that magnetars can power some short gamma-ray bursts.

引用

页码：385 / +

页数：14

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