Rise and fall of the high-energy afterglow emission of GRB 180720B

被引：20

作者：

Ronchi, M. ^{[1
]}

Fumagalli, F. ^{[1
]}

Ravasio, M. E. ^{[1
]}

Oganesyan, G. ^{[2
,3
,4
]}

Toffano, M. ^{[5
,6
]}

Salafia, O. S. ^{[6
,7
]}

Nava, L. ^{[6
,8
,9
]}

Ascenzi, S. ^{[6
]}

Ghirlanda, G. ^{[6
,7
]}

Ghisellini, G. ^{[6
]}

机构：

[1] Univ Milano Bicocca, Dip Fis G Occhialini, Piazza Sci 3, I-20126 Milan, Italy

[2] Gran Sasso Sci Inst, Viale F Crispi 7, I-67100 Laquila, Italy

[3] Ist Nazl Fis Nucl, Lab Nazl Gran Sasso, I-67100 Laquila, Italy

[4] INAF Osservatorio Astron Abruzzo, Via M Maggini SNC, I-64100 Teramo, Italy

[5] Univ Insubria, Via Valleggio 11, I-22100 Como, Italy

[6] INAF Osservatorio Astron Brera, Via E Bianchi 46, I-23807 Merate, Italy

[7] Ist Nazl Fis Nucl, Sez Milano Bicocca, Piazza Sci 3, I-20126 Milan, Italy

[8] Ist Nazl Fis Nucl, Sez Trieste, Via Valerio 2, I-34149 Trieste, Italy

[9] IFPU, I-34151 Trieste, Italy

来源：

ASTRONOMY & ASTROPHYSICS | 2020年 / 636卷

关键词：

gamma-ray burst: general; radiation mechanisms: non-thermal; relativistic processes; acceleration of particles; GAMMA-RAY BURSTS; X-RAY; RELATIVISTIC SHOCKS; INTERNAL SHOCKS; TELESCOPE; MODELS; ACCELERATION; CONSTRAINTS; VARIABILITY; CURVES;

D O I：

10.1051/0004-6361/201936765

中图分类号：

P1 [天文学];

学科分类号：

0704 ;

摘要：

The gamma-ray burst (GRB) 180720B is one of the brightest events detected by the Fermi satellite and the first GRB detected by the H.E.S.S. telescope above 100 GeV, at around ten hours after the trigger time. We analysed the Fermi (GBM and LAT) and Swift (XRT and BAT) data and describe the evolution of the burst spectral energy distribution in the 0.5 keV-10 GeV energy range over the first 500 s of emission. We reveal a smooth transition from the prompt phase, dominated by synchrotron emission in a moderately fast cooling regime, to the afterglow phase whose emission has been observed from the radio to the gigaelectronvolts energy range. The LAT (0.1-100 GeV) light curve initially rises (F-LAT proportional to t(2.4)), peaks at similar to 78 s, and falls steeply (F-LAT proportional to t(-2.2)) afterwards. The peak, which we interpret as the onset of the fireball deceleration, allows us to estimate the bulk Lorentz factor Gamma (0)similar to 150 (300) under the assumption of a circum-burst medium with a wind-like (homogeneous) density profile. We derive a flux upper limit in the LAT energy range at the time of H.E.S.S. detection, but this does not allow us to unveil the nature of the high-energy component observed by H.E.S.S. We fit the prompt spectrum with a physical model of synchrotron emission from a non-thermal population of electrons. The 0-35 s spectrum after its EF(E) peak (at 1-2 MeV) is a steep power law extending to hundreds of megaelectronvolts. We derive a steep slope of the injected electron energy distribution N(gamma) proportional to gamma (-5). Our fit parameters point towards a very low magnetic field (B ' similar to 1 G) in the emission region.

引用

页数：10

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