玛射线爆发的早期光学极化发生后的光
Carole G Mundell1, Iain A Steele, Robert J Smith
1Astrophysics Research Institute, Liverpool John Moores University, Twelve Quays House, Egerton Wharf, Birkenhead, CH41 1LD, UK. cgm@astro.livjm.ac.uk
概括
我们测量了玛射线爆发的光学偏振. 在光开始时的低极化排除了标准马射线爆发模型中大规模的磁场.
科学领域:
- 天体物理学 天体物理学
- 高能天文学 高能天文学
背景情况:
- 马射线爆炸 (GRB) 是宇宙中最明亮的爆炸.
- 了解GRB的发射机制和磁场结构对于测试理论模型至关重要.
研究的目的:
- 为了研究马射线爆发 (GRB) 的光学偏振,后光.
- 为了限制GRB发射区域的磁场特性.
主要方法:
- 用机器人利物浦望远镜上的环极度计测量GRB 060418的光学偏振.
- 对偏振数据的分析与后照亮亮度衰减率的结合.
主要成果:
- 在GRB发生203秒后,获得了不到8%的极化强大的上限.
- 这种低极化与火球减速时间一致.
结论:
- 观察到的低极化和衰变速度限制了标准的GRB喷射模型.
- 结果排除了在GRB 060418.18发射区域存在大规模有序磁场的可能性.
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