聚合后的毫秒脉冲星产生的X射线耀斑.
1Department of Astronomy, Nanjing University, Nanjing 210093, China. dzg@nju.edu.cn
概括
短时间的马射线爆发可能来自于合并的中子星. 新形成的脉冲星可以在合并事件后通过磁场相互作用产生持久的X射线耀斑.
科学领域:
- 天体物理学 天体物理学
- 高能天体物理学 高能天体物理学
- 紧型对象的合并 紧型对象的合并
背景情况:
- 最近的观测表明,短时间的马射线爆发 (GRBs) 是由紧的恒星合并产生的.
- 在短时间的GRB中观察到的X射线耀斑比先前的合并后模型预测的持续时间更长.
研究的目的:
- 为了研究短短的马射线爆发后扩展的X射线耀斑的起源.
- 提出一种机制,涉及二进制中子星合并中的合并后现象.
主要方法:
- 利用不同旋转的理论建模,在双中子恒星合并后形成的毫秒脉冲星.
- 分析磁场的演变,包括极形磁场的起和圆形磁场的产生.
- 调查磁重新连接的过程和随后的爆炸事件.
主要成果:
- 新形成的脉冲星的微分旋转可以显著放大内部磁场.
- 由恒星表面产生的强大的圆形磁场可以从恒星表面出现.
- 这些新出现的磁场的磁再连接可以驱动爆炸事件,产生X射线火焰.
结论:
- 不同旋转的毫秒脉冲星为短时间GRB后观察到的长时间X射线耀斑提供了可行的解释.
- 拟议的机制将观察到的耀斑持续时间与合并后的理论时间尺度相协调.
- 这项研究为中子星合并后的能量过程提供了新的视角.
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