VERY HIGH ENERGY γ-RAY AFTERGLOW EMISSION OF NEARBY GAMMA-RAY BURSTS

被引：13

作者：

Xue, R. R. ^{[1
,2
]}

Tam, P. H. ^{[3
]}

Wagner, S. J. ^{[3
]}

Behera, B. ^{[3
]}

Fan, Y. Z. ^{[1
,4
]}

Wei, D. M. ^{[1
,5
]}

机构：

[1] Chinese Acad Sci, Purple Mt Observ, Nanjing 210008, Peoples R China

[2] Chinese Acad Sci, Grad Sch, Beijing 100012, Peoples R China

[3] Univ Heidelberg, D-6900 Heidelberg, Germany

[4] Univ Copenhagen, Niels Bohr Inst, Niels Bohr Int Acad, DK-2100 Copenhagen, Denmark

[5] Nanjing Univ, Purple Mt Observ, Joint Ctr Particle Nucl Phys & Cosmol, Nanjing 210008, Peoples R China

来源：

ASTROPHYSICAL JOURNAL | 2009年 / 703卷 / 01期

基金：

新加坡国家研究基金会; 美国国家科学基金会;

关键词：

gamma rays: bursts; ISM: jets and outflows; radiation mechanisms: non-thermal; INVERSE COMPTON EMISSION; LIGHT CURVES; HOST GALAXY; OPTICAL AFTERGLOW; HESS OBSERVATIONS; LONG-DURATION; UPPER LIMITS; SWIFT; GRB-030329; COMPONENT;

D O I：

10.1088/0004-637X/703/1/60

中图分类号：

P1 [天文学];

学科分类号：

0704 ;

摘要：

The synchrotron self-Compton (SSC) emission from gamma-ray burst (GRB) forward shock can extend to the very high energy (VHE; E gamma > 100 GeV) range. Such high energy photons are rare and are attenuated by the cosmic infrared background before reaching us. In this work, we discuss the prospect to detect these VHE photons using the current ground-based Cherenkov detectors. Our calculated results are consistent with the upper limits obtained with several Cherenkov detectors for GRB 030329, GRB 050509B, and GRB 060505 during the afterglow phase. For five bursts in our nearby GRB sample (except for GRB 030329), current ground-based Cherenkov detectors would not be expected to detect the modeled VHE signal. Only for those very bright and nearby bursts like GRB 030329, detection of VHE photons is possible under favorable observing conditions and a delayed observation time of less than or similar to 10 hr.

引用

页码：60 / 67

页数：8

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