AJELLO, M.; ARIMOTO, M.; ASANO, K.; AXELSSON, M.; BALDINI, L.; BARBIELLINI, G.; BASTIERI, D.; BELLAZZINI, R.; BERRETTA, A.; BISSALDI, E.; BLANDFORD, R.D.; BONINO, R.; BOTTACINI, E.; BREGEON, J.; BRUEL, P.; BUEHLER, R.; BUSON, S.; CAMERON, R.A.; CAPUTO, R.; CARAVEO, P.A.; CAVAZZUTI, E.; CHEN, S.; CHIARO, G.; CIPRINI, S.; COSTANTIN, D.; CUTINI, S.; D'AMMANDO, F.; TORRE LUQUE, P. De La; DE PALMA, F.; LALLA, N.Di; VENERE, L.Di; DIRIRSA, F.Fana; FEGAN, S.J.; FRANCKOWIAK, A.; FUKAZAWA, Y.; FUSCO, P.; GARGANO, F.; GASPARRINI, D.; GIGLIETTO, N.; GIORDANO, F.; GIROLETTI, M.; GREEN, D.; GRENIER, I.A.; GRONDIN, M.H.; GUIRIEC, S.; HAYS, E.; HORAN, D.; JÓHANNESSON, G.; KOCEVSKI, D.; KOVACEVIC, M.; KUSS, M.; LARSSON, S.; LATRONICO, L.; LI, J.; LIODAKIS, I.; LONGO, F.; LOPARCO, F.; LOVELLETTE, M.N.; LUBRANO, P.; MALDERA, S.; MANFREDA, A.; MARTÍ-DEVESA, G.; MAZZIOTTA, M.N.; MCENERY, J.E.; MEREU, I.; MICHELSON, P.F.; MIZUNO, T.; MONZANI, M.E.; MORETTI, E.; MORSELLI, A.; MOSKALENKO, I.V.; NEGRO, M.; NUSS, E.; OHNO, M.; OMODEI, N.; ORIENTI, M.; ORLANDO, E.; PALATIELLO, M.; PALIYA, V.S.; PANEQUE, D.; PEI, Z.; PERSIC, M.; PESCE-ROLLINS, M.; PETROSIAN, V.; PIRON, F.; POON, H.; PORTER, T.A.; PRINCIPE, G.; RACUSIN, J.L.; RAINÒ, S.; RANDO, R.; RANI, B.; RAZZANO, M.; REIMER, A.; REIMER, O.; SERINI, D.; SGRÒ, C.; SISKIND, E.J.; SPANDRE, G.; SPINELLI, P.; TAJIMA, H.; TAKAGI, K.; TAK, Donggeun; TORRES, D.F.; VALVERDE, J.; WOOD, K.; YAMAZAKI, R.; YASSINE, M.; ZHU, S.; UHM, Z. Lucas; ZHANG, Bing

doi:10.3847/2041-8213/ab564f

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Astrophys.J.. 2019, vol. 886, n° 2, p. L33

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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 γ-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 γ-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, 1.7 × 10−6 erg cm−2. The total fluence from three γ-ray flares is 5.3 × 10−6 erg cm−2. The three γ-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 ( = 2 + ), which is the first observational evidence of the high-latitude emission in the GeV energy band.< Réduire

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gamma rays bursts

GRB131108A

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Bright Gamma-Ray Flares Observed in GRB 131108A

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