冷却和加热固体夸克星
Cooling and Heating Solid Quark Stars
摘要：
本文提出一个唯象的固体夸克星脉冲星模型来解释观测到的孤立夸克星的热X射线辐射。固体夸克星的热容量被发现相当小，因此在恒星诞生时获得的残余内部恒星热量可以在极短的时间尺度内消散。然而，回流等离子体在固体夸克星的两极引起的轰击会使恒星被重新加热，从而可以维持长期的软X射线发射。这种设想可用于那些具有显著磁层活动的X射线天体，从而确定它们的冷却过程。暗X射线孤立中子星（XDIN）以及致密中心天体（CCO）已被观测到，软X射线辐射占主导地位，磁层表现很少。这种来源可能是在螺旋桨状态下吸积的固体夸克星。
英文摘要：
We present here a phenomenological solid quark star pulsar model to interpret the observed thermal X-ray emission of isolated pulsars. The heat capacity for solid quark stars was found to be quite small, so that the residual internal stellar heat gained at the birth of the star could be dissipated in an extremely short timescale. However, the bombardment induced by backflowing plasma at the poles of solid quark stars would get the stars be reheated, so that long term soft X-ray emission can be sustained. Such a scenario could be used for those X-ray pulsars with significant magnetospheric activities, and their cooling processes would thus be established. Dim X-ray isolated neutron stars (XDINs) as well as compact central objects (CCOs) have been observed with dominant soft X-ray radiation combined with little magnetospheric manifestations. Such sources could be solid quark stars accreting in the propeller regime.
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