标题： 吸积中子星的热释放 显示英文标题

标题： Heat release in accreting neutron stars

摘要： 吸积中子星（NS）在安静状态下的热辐射被认为是由非平衡核反应加热恒星外壳引起的（深壳加热范式）。 我们推导了一个简单的普适公式来表示加热效率，假设中子星有一个完全吸积的外壳。 我们进一步表明，在最近提出的热力学一致的吸积壳方法中，热量释放可以由单一参数——外内壳界面的压力 $P_{\rm oi}$ 来参数化（我们认为这个压力不一定与中子滴落压力重合）。 我们讨论了几种考虑壳效应的核模型的 $P_{\rm oi}$ 可能值，并确定了净热量释放及其在壳内的分布作为 $P_{\rm oi}$ 的函数。 我们得出结论，与之前的工作相比，热量释放应该减少几倍。 显示英文摘要

摘要： Observed thermal emission from accreting neutron stars (NSs) in a quiescent state is believed to be powered by nonequilibrium nuclear reactions that heat the stellar crust (deep crustal heating paradigm). We derive a simple universal formula for the heating efficiency, assuming that an NS has a fully accreted crust. We further show that, within the recently proposed thermodynamically consistent approach to the accreted crust, the heat release can be parametrized by the only one parameter -- the pressure $P_{\rm oi}$ at the outer-inner crust interface (as we argue, this pressure should not necessarily coincide with the neutron-drip pressure). We discuss possible values of $P_{\rm oi}$ for a selection of nuclear models that account for shell effects, and determine the net heat release and its distribution in the crust as a function of $P_{\rm oi}$. We conclude that the heat release should be reduced by a factor of few in comparison to previous works.