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Bright Gamma-Ray Flares Observed in GRB 131108A
Clemson Univ, Kinard Lab Phys, Dept Phys & Astron, Clemson, SC 29634 USA..
Kanazawa Univ, Inst Sci & Engn, Fac Math & Phys, Kanazawa, Ishikawa 9201192, Japan..
Univ Tokyo, Inst Cosm Ray Res, 5-1-5 Kashiwanoha, Kashiwa, Chiba 2778582, Japan..
KTH, School of Engineering Sciences (SCI), Physics, Particle and Astroparticle Physics. Stockholm Univ, AlbaNova, Dept Phys, SE-10691 Stockholm, Sweden.ORCID iD: 0000-0003-4378-8785
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2019 (English)In: Astrophysical Journal Letters, ISSN 2041-8205, E-ISSN 2041-8213, Vol. 886, no 2, article id L33Article in journal (Refereed) Published
Abstract [en]

GRB 131108A is a bright long gamma-ray burst (GRB) detected by the Large Area Telescope and the Gamma-ray Burst Monitor on board the Fermi Gamma-ray Space Telescope. Dedicated temporal and spectral analyses reveal three ?-ray flares dominating above 100 MeV, which are not directly related to the prompt emission in the Gamma-ray Burst Monitor band (10 keV?10 MeV). The high-energy light curve of GRB 131108A (100 MeV?10 GeV) shows an unusual evolution: a steep decay, followed by three flares with an underlying emission, and then a long-lasting decay phase. The detailed analysis of the ?-ray flares finds that the three flares are 6?20 times brighter than the underlying emission and are similar to each other. The fluence of each flare, (1.6?2.0)10(?6) erg cm(?2), is comparable to that of emission during the steep decay phase, 1.710(?6) erg cm(?2). The total fluence from three ?-ray flares is 5.310(?6) erg cm(?2). The three ?-ray flares show properties similar to the usual X-ray flares that are sharp flux increases, occurring in ?50% of afterglows, in some cases well after the prompt emission. Also, the temporal and spectral indices during the early steep decay phase and the decaying phase of each flare show the consistency with a relation of the curvature effect (<CDATA<i=2 + <CDATA<i), which is the first observational evidence of the high-latitude emission in the GeV energy band.

Place, publisher, year, edition, pages
Institute of Physics (IOP), 2019. Vol. 886, no 2, article id L33
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Physical Sciences
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URN: urn:nbn:se:kth:diva-265507DOI: 10.3847/2041-8213/ab564fISI: 000499346800001Scopus ID: 2-s2.0-85077649318OAI: oai:DiVA.org:kth-265507DiVA, id: diva2:1379546
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QC 20191217

Available from: 2019-12-17 Created: 2019-12-17 Last updated: 2020-02-04Bibliographically approved

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