在一个不断增长的毫秒脉冲星中,近周期性的X射线亮度波动
R Wijnands1, M Van Der Klis, J Homan
1School of Physics and Astronomy, University of St Andrews, North Haugh, St Andrews, Fife KY16 9SS, UK. radw@st-andrews.ac.uk
Nature
|July 4, 2003
概括
研究人员将千赫兹准周期性振荡 (kHz QPOs) 与中子星旋转频率联系起来. 这一发现挑战了现有的模型,并需要一种新的方法来理解在积中子星中的这些现象.
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
- 中子星物理学 中子星物理学
背景情况:
- 相对论等离子体流向聚合中子星提供了对强场引力和超核密度内部的洞察.
- X射线亮度波动,特别是双千赫兹准周期性振荡 (kHz QPOs),源于中子星附近的等离子体异质性.
研究的目的:
- 为了研究kHz QPOs和中子星旋转频率之间的关系.
- 为了测试现有的kHz QPO生成模型.
主要方法:
- 来自具有已知自旋频率的中子星的kHz QPOs的检测.
- 分析X射线亮度波动以确定QPO频率.
主要成果:
- 在kHz QPOs和中子星的旋转频率之间建立了明确的相关性.
- 目前的理论模型并不能预测观察到的关系.
结论:
- 现有的kHz QPO模型不足以解释观察到的旋转-QPO关系.
- 要了解kHz QPOs,需要一个新的理论框架,可能涉及旋转和相对论频率之间的共振.
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