无线电毫秒脉冲星在起源时的回转下降
1Argelander-Institut für Astronomie, Universität Bonn, Bonn, Germany. tauris@astro.uni-bonn.de
概括
来自中子星的制动扭矩.
科学领域:
- * 天体物理学 * 天体物理学
- * 恒星进化过程中的恒星进化
- * 中子星物理学
背景情况:
- *毫秒脉冲星是旧的中子星,由二进制伴星的质量积累旋转而形成.
- * 了解早期的旋转进化需要分析在质量转移终止期间膨胀的磁层.
研究的目的:
- * 为了研究膨胀的磁层对中子星旋转进化的影响.
- *为了解释旋转分布的观察差异和毫秒脉冲星的年龄差异.
主要方法:
- * 进行了二进制恒星演变计算.
- *分析了伴星罗氏叶断后中子星的制动扭矩.
主要成果:
- * 制动扭矩可以消散超过50%的脉冲星的旋转能量.
- *这种能量消散可能解释X射线脉冲星和无线电脉冲星之间的自旋分布差异.
结论:
- * 制动扭矩机制对于理解毫秒脉冲星旋转演变至关重要.
- * 这种机制可能会解决脉冲星旋转分布和年龄估计的差异.
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