Magnetic jet model for GRBs and the delayed arrival of > 100MeV photons

被引：19

作者：

Bosnjak, Z. ^{[1
]}

Kumar, P. ^{[2
]}

机构：

[1] Univ Paris Diderot, UMR 7158, AIM,CEA,DSM,CNRS, Irfu Serv Astrophys, F-91191 Gif Sur Yvette, France

[2] Univ Texas Austin, Dept Astron, Austin, TX 78712 USA

来源：

MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY | 2012年 / 421卷 / 01期

基金：

美国国家科学基金会;

关键词：

radiation mechanisms: non-thermal; methods: analytical; gamma-ray burst: general; GAMMA-RAY BURSTS; INTERNAL SHOCK MODEL; HIGH-ENERGY EMISSION; FERMI OBSERVATIONS; SPECTRAL COMPONENT; ACCELERATION; PROMPT; RADIATION; DISSIPATION; AFTERGLOW;

D O I：

10.1111/j.1745-3933.2011.01202.x

中图分类号：

P1 [天文学];

学科分类号：

0704 ;

摘要：

Photons of energy larger than 100MeV from long GRBs arrive a few seconds after < 10MeV photons do. We show that this delay is a natural consequence of a magnetic-dominated relativistic jet. The much slower acceleration of a magnetic jet with radius (compared with a hot baryonic outflow) results in high-energy. gamma-ray photons to be converted to electron-positron pairs out to a larger radius, whereas lower energy. gamma-rays of energy less than similar to 10MeV can escape when the jet crosses the Thomson photosphere. The resulting delay for the arrival of high-energy photons is found to be similar to the value observed by the Fermi satellite for a number of GRBs. A prediction of this model is that the delay should increase with photon energy (E) as similar to E-0.17 for E > 100MeV. The delay depends almost linearly on burst redshift, and on the distance from the central compact object where the jet is launched (R-0). Therefore, the delay in arrival of > 10(2) MeV photons can be used to estimate burst redshift if the magnetic jet model for. gamma-ray generation is correct and R-0 is roughly the same for long GRBs.

引用

页码：L39 / L43

页数：5

共 42 条

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Magnetic jet model for GRBs and the delayed arrival of &gt; 100MeV photons

Magnetic jet model for GRBs and the delayed arrival of > 100MeV photons