一个非常高能量的组件深处的γ射线爆发后光
H Abdalla1, R Adam2, F Aharonian3,4,5
1Centre for Space Research, North-West University, Potchefstroom, South Africa.
Nature
|November 22, 2019
概括
从玛射线爆发 (GRBs) 检测到非常高能量的辐射深处的后光阶段. 这一发现挑战了现有的模型,并表明反复的康普顿辐射可能解释了这些高能量的宇宙爆炸的晚期辐射.
科学领域:
- 天体物理学
- 高能天体物理学
- 太空爆炸
背景情况:
- 马射线爆发是宇宙中最有活力的爆炸现象.
- GRB的发射包括快速和后照相,后照相显示亮度逐渐下降.
- 来自GRB的高能光子 (GeV) 被检测到,但它们的起源和非常高能 (VHE) 辐射仍然不清楚.
研究的目的:
- 研究来自玛射线爆发的非常高能光子的起源.
- 在GRB后发光阶段分析VHE辐射的发射机制.
主要方法:
- 在GRB 180720B的后发光阶段观察到非常高能 (VHE) 辐射.
- 在X射线和马射线范围内分析能量流和光子指数.
- 将观察到的数据与反向康普顿和同步发射的理论模型进行比较.
主要成果:
- 在即时发射结束10小时后检测到GRB 180720B的VHE发射.
- 在X射线和马射线范围内观察到可比的能量流和光子指数.
- 反向康普顿排放模型减轻了晚期VHE排放的粒子能量需求.
结论:
- 在GRB后发光的深处检测VHE发射对GRB环境和发射机制提供了关键的约束.
- 反向康普顿散射是晚期VHE发射的一个合理解释,缓解粒子能量需求.
- 这一发现对未来的VHE对马射线爆发的观测有重要意义.
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