Fate of the companion stars of ultra-rapid pulsars
Fate of the companion stars of ultra-rapid pulsars
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DOI：
10.1038/334227a0
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发表时间：
1988-07
期刊：
影响因子：
64.8
通讯作者：
E. V. Heuvel;J. Paradijs
中科院分区：
文献类型：
--
作者：
E. V. Heuvel;J. Paradijs
一颗毫秒脉冲星是在双星系统中通过自旋向上的“再循环”形成的，一旦质量传递暂时中断，由于大的脉冲星能量流的撞击，它的伴星星星就会开始蒸发。如果脉冲星的脉冲周期很短，伴星星星的半径相对较大，因此富含氢，并且轨道周期很短，这种蒸发是最容易的。毫秒射电双星引起的伴星蒸发可以解释为什么在激变变星的周期间隔以下缺乏轨道周期短的低质量X射线双星，以及新生射电双星及其空间速度的统计数据。
A millisecond pulsar that is formed by spin-up 'recycling'1,2in a binary system will, once the mass transfer becomes temporarily interrupted, start to evaporate its companion star as a consequence of the large impinging pulsar energy flux. This evaporation is easiest if the pulsar has a short pulse period, the companion star has a relatively large radius and is therefore hydrogen-rich, and the orbital period is short. Evaporation of companion stars induced by millisecond pulsars could account for the lack of low-mass X-ray binaries with short orbital periods below the period gap of the cataclysmic variables, and for the statistics of new-born radio pulsars and their space velocities.