标题： 暂积增殖中子星的热状态 显示英文标题

标题： Thermal state of transiently accreting neutron stars

摘要： 我们研究了暂时吸积的中子星（平均吸积率 $\dot{M} \sim 10^{-14}-10^{-9}$ M$_\odot$ 年$^{-1}$）的热状态，这些热状态由吸积物质下沉进入恒星内部时的深部壳层加热所决定。 我们将此问题直接对应于冷却中子星的问题进行了形式化。 利用一个简单的玩具模型，我们分析了影响吸积恒星热状态的最重要因素：低质量恒星核心中的强超流性和高质量恒星核心中的快速中微子发射（在核物质、pion凝聚、kaon凝聚或夸克相中）。 我们简要地将结果与软X射线暂现源在平静期的观测进行了比较。 如果在SAX J1808.4-3658中子星（Campana 等人，2002年）的平静期热发光上限与深部壳层加热相关，则它支持开启了直接Urca过程的核子中子星核模型。 显示英文摘要

摘要： We study thermal states of transiently accreting neutron stars (with mean accretion rates $\dot{M} \sim 10^{-14}-10^{-9}$ M$_\odot$ yr$^{-1}$) determined by the deep crustal heating of accreted matter sinking into stellar interiors. We formalize a direct correspondence of this problem to the problem of cooling neutron stars. Using a simple toy model we analyze the most important factors which affect the thermal states of accreting stars: a strong superfluidity in the cores of low-mass stars and a fast neutrino emission (in nucleon, pion-condensed, kaon-condensed, or quark phases of dense matter) in the cores of high-mass stars. We briefly compare the results with the observations of soft X-ray transients in quiescence. If the upper limit on the quiescent thermal luminosity of the neutron star in SAX J1808.4-3658 (Campana et al. 2002) is associated with the deep crustal heating, it favors the model of nucleon neutron-star cores with switched-on direct Urca process.