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核动力毫秒脉冲星和中子星的最大旋转频率
Deepto Chakrabarty1, Edward H Morgan, Michael P Muno
1Department of Physics and Center for Space Research, Massachusetts Institute of Technology, Cambridge, Massachusetts 02139, USA. deepto@space.mit.edu
Nature
|July 4, 2003
概括
增加的毫秒脉冲星.
科学领域:
- 天体物理学 天体物理学
- X射线天文学X射线天文学
- 中子星物理学 中子星物理学
背景情况:
- 毫秒脉冲星是快速旋转的中子星,由伴星的质量积累形成.
- 热核X射线爆发是由于核燃烧不稳定而导致中子星的积累而观察到的.
- 爆发期间的毫秒周期亮度振荡以前被认为表明恒星自转,但缺乏直接证据.
研究的目的:
- 为了提供直接证明激增毫秒脉冲星中爆发振荡的旋转起源.
- 为了确认爆发振荡准确地测量中子星的旋转.
- 研究核动力脉冲星的旋转频率分布,并测试理论模型.
主要方法:
- 检测爆发振荡在已知的旋转频率的增量毫秒脉冲星.
- 分析这些振荡的旋转相一致性.
- 检查了11颗核动力脉冲星的旋转频率.
主要成果:
- 探测到的爆发振荡与已知的旋转频率精确匹配,与一个增长的毫秒脉冲星相匹配.
- 这些振荡始终保持着相同的旋转阶段.
- 观察到的核动力脉冲星的自旋频率被发现远低于理论分解极限.
结论:
- 爆发振荡被证实是核动力脉冲,直接追踪积聚中子星的旋转.
- 重力辐射损失被支持作为一种限制增积扭矩和在毫秒脉冲星中的自转的机制.
- 这些发现证实了关于中子星旋转演变的理论预测.
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