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arXiv 0808.3485astro-ph
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一种新的射电脉冲星-早在1982年

A New Class of Radio Pulsars - Back in 1982

M. Ali Alpar

备注：
Invited review, to appear in the proceedings of the workshop 'A Decade of Accreting Millisecond X-ray Pulsars' (Amsterdam, April 2008). Dedicated to the memory of Jacob Shaham, who knew millisecond X-ray pulsars would be discovered one day
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摘要：

关于中子星上的力矩和平衡自转周期的存在的基本想法是从认识到大多数X射线双星包含吸积动力的中子星开始的。双星通过吸积阶段演化到中子星上，最终导致吸积后的射电脉冲星阶段，最初被讨论作为一种方法来理解射电脉冲星中双星的稀缺性，以及第一批发现的双星射电脉冲星相对较短的旋转周期，其磁场小于熟悉的$10^{12} G$范围。毫秒射电星的发现使我们意识到，在一类新的射电星中，由于LMXB的吸积作用而产生的场可以低得多。预测的毫秒脉冲星的自旋下降率很快得到了证实。观测者们对毫秒X射线周期的探索开始了，首先导致了QPO的发现，并最终导致了X射线毫秒双星的发现。理论家们对为什么没有从LMXB中观察到X射线毫秒脉动的解释也立即开始了。

英文摘要：

Basic ideas about the torques on the neutron star and the existence of an equilibrium rotation period followed from the recognition that most X-ray binaries contain accretion powered neutron stars. The evolution of binaries through a phase of accretion onto the neutron star, eventually leading to a post-accretion radio pulsar phase, was initially discussed as a way to understand the scarcity of binaries among the radio pulsars and the relatively short rotation periods of the first discovered binary radio pulsars in terms of magnetic fields that would be smaller than the familiar $10^{12} G$ range. The discovery of the millisecond pulsars made us realize that the fields can be much lower in a new class of radio pulsars that have been spun up by accretion in LMXBs. The predicted spin-down rates of the millisecond pulsar was soon confirmed. The observers' search for millisecond X-ray periods was on, leading first to the discovery of QPOs, and eventually to the discovery of the X-ray millisecond pulsars. The theorists' quest for explanations of why X-ray millisecond pulsations are not observed from LMXBs also started right away.

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