He, Hao-Ning 2009 低光度暴的高能辐射

主要内容:
考虑SSC和EIC

精彩摘抄:


文章信息:

· Find Similar Abstracts (with default settings below)

· Electronic Refereed Journal Article (HTML)

· Full Refereed Journal Article (PDF/Postscript)

· arXiv e-print (arXiv:0911.4217)

· References in the article

· Citations to the Article (1) (Citation History)

· Refereed Citations to the Article

· SIMBAD Objects (7)

· Also-Read Articles (Reads History)

·

· Translate This Page

Title:		High-energy Gamma-ray Afterglows from Low-luminosity Gamma-ray Bursts
Authors:		He, Hao-Ning; Wang, Xiang-Yu; Yu, Yun-Wei; Mészáros, Peter
Affiliation:		AA(Department of Astronomy, Nanjing University, Nanjing 210093, China ), AB(Department of Astronomy, Nanjing University, Nanjing 210093, China ; Key Laboratory for Particle Astrophysics, Institute of High Energy Physics, Chinese Academy of Sciences, Beijing 100049, China), AC(Department of Astronomy, Nanjing University, Nanjing 210093, China ; Institute of Astrophysics, Huazhong Normal University, Wuhan 430079, China ), AD(Department of Astronomy and Astrophysics, Pennsylvania State University, University Park, PA 16802, USA ; Department of Physics, Pennsylvania State University, University Park, PA 16802, USA )
Publication:		The Astrophysical Journal, Volume 706, Issue 2, pp. 1152-1162 (2009). (ApJ Homepage)
Publication Date:		12/2009
Origin:		IOP
ApJ Keywords:		gamma rays: bursts
DOI:		10.1088/0004-637X/706/2/1152
Bibliographic Code:		2009ApJ...706.1152H

Abstract

The observations of gamma-ray bursts (GRBs) such as 980425, 031203 and 060218, with luminosities much lower than those of other classic bursts, lead to the definition of a new class of GRBs—LL-GRBs. The nature of the outflow responsible for them is not yet clear. Two scenarios have been suggested: one is the conventional relativistic outflow with initial Lorentz factor of order of Γ₀ gsim 10 and the other is a trans-relativistic outflow with Γ₀ sime 1-2. Here, we compare the high-energy gamma-ray afterglow emission from these two different models, taking into account both synchrotron self-inverse Compton (SSC) scattering and the external inverse Compton scattering due to photons from the cooling supernova or hypernova envelope (SNIC). We find that the conventional relativistic outflow model predicts a relatively high gamma-ray flux from SSC at early times (<10⁴ s for typical parameters) with a rapidly decaying light curve, while in the trans-relativistic outflow model, one would expect a much flatter light curve of high-energy gamma-ray emission at early times, which could be dominated by both the SSC emission and the SNIC emission, depending on the properties of the underlying supernova and the shock parameter epsilon _e and epsilon _B . The Fermi Gamma-ray Space Telescope should be able to distinguish between the two models in the future.

---

Bibtex entry for this abstract   Preferred format for this abstract (see Preferences)