Gamma-ray burst afterglow blast waves

被引：22

作者：

van Eerten, Hendrik ^{[1
]}

机构：

[1] Univ Bath, Dept Phys, Bath BA2 7AY, Avon, England

来源：

INTERNATIONAL JOURNAL OF MODERN PHYSICS D | 2018年 / 27卷 / 13期

关键词：

Gamma-ray bursts; HIGH-ENERGY EMISSION; RAYLEIGH-TAYLOR INSTABILITY; MAGNETAR CENTRAL ENGINES; LARGE-AREA TELESCOPE; LIGHT CURVES; RELATIVISTIC JETS; FERMI OBSERVATIONS; LORENTZ FACTORS; REVERSE SHOCK; GRB; 130427A;

D O I：

10.1142/S0218271818420026

中图分类号：

P1 [天文学];

学科分类号：

0704 ;

摘要：

The various stages of baryonic gamma-ray burst (GRB) afterglow blast waves are reviewed. These are responsible for the afterglow emission from which much of our understanding of gamma-ray bursts derives. Initially, the blast waves are confined to the dense medium surrounding the burster (stellar envelope or dense wind), giving rise to a jet-cocoon structure. A massive ejecta is released and potentially fed by ongoing energy release from the burster and a forward-reverse shock system is set up between ejecta and ambient density. Ultimately the blast wave spreads sideways and slows down, and the dominant afterglow emission shifts from X-rays down to radio. Over the past years significant progress has been made both observationally and theoretically/numerically in our understanding of these blast waves, unique in the universe due to their often incredibly high initial Lorentz factors of 100-1000. The recent discovery of a short gamma-ray burst counterpart to a gravitational wave detection (GW 170817) brings the promise of a completely new avenue to explore and constrain the dynamics of gamma-ray burst blast waves.

引用

页数：46

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