A model for delayed emission in a very-high energy gamma-ray flare in Markarian 501

被引：22

作者：

Bednarek, W. ^{[1
]}

Wagner, R. M. ^{[2
]}

机构：

[1] Univ Lodz, Dept Expt Phys, PL-90236 Lodz, Poland

[2] Max Planck Inst Phys & Astrophys, D-80805 Munich, Germany

来源：

ASTRONOMY & ASTROPHYSICS | 2008年 / 486卷 / 03期

关键词：

galaxies : active; BL Lacertae objects : individual : Mrk 501; radiation mechanisms : non-thermal; gamma rays : theory;

D O I：

10.1051/0004-6361:20079068

中图分类号：

P1 [天文学];

学科分类号：

0704 ;

摘要：

Context. Recently, the MAGIC collaboration reported evidence for a delay in the arrival times of photons of different energies during a.-ray flare from the blazar Markarian 501 on 2005 July 9. Aims. We aim at describing the observed delayed high-energy emission. Methods. We apply a homogeneous synchrotron self-Compton (SSC) model under the assumption that the blob containing relativistic electrons was observed in its acceleration phase. Results. This modified SSC model predicts the appearance of a gamma-ray flare first at lower energies and subsequently at higher energies. Conclusions. Based on the reported time delay of similar to 240 s between the flare observed at similar to 190GeV and 2.7 TeV, we predict a delay on the order of 1 h if observed between 10GeV and 100GeV. Such delay timescales can be tested in the future by simultaneous flare observations with the Gamma Ray Large Area Space Telescope (GLAST) and Cherenkov telescopes.

引用

页码：679 / 682

页数：4

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