论文标题
爆发中子星的外壳中的热扩散模型
Model of heat diffusion in the outer crust of bursting neutron stars
论文作者
论文摘要
我们研究了能量释放后的热扩散，在外侧恒星外壳的深球层中（10^7 <ρ<4 x 10^{11} g/cm^3）。我们证明，该层具有特定的热蓄能特性，吸收热量并主要将其引导到恒星内。由于其高热容量，它可以吸收约10^{43} -10^{44} ERG，直到其温度超过T〜3 x 10^9 K并触发快速中微子冷却。带有T〜10^8-3 x 10^9 K的温暖层可以用作良好的热储层，该储层与内皮和恒星芯热脱钩几个月。我们提出了一个玩具模型，以探索热蓄积层中的热扩散，并使用数值模拟测试该模型。我们制定了热传播的一些通用特征，例如在积聚中子恒星中对超级爆炸的解释。我们对这种超级爆炸后的余辉进行了相似的分析，这可能有助于估计爆发恒星的特性。
We study heat diffusion after an energy release in a deep spherical layer of the outer neutron star crust (10^7 < ρ< 4 x 10^{11} g/cm^3). We demonstrate that this layer possesses specific heat-accumulating properties, absorbing heat and directing it mostly inside the star. It can absorb up to about 10^{43}-10^{44} erg due to its high heat capacity, until its temperature exceeds T ~ 3 x 10^9 K and triggers a rapid neutrino cooling. A warm layer with T ~ 10^8 - 3 x 10^9 K can serve as a good heat reservoir, which is thermally decoupled from the inner crust and the stellar core for a few months. We present a toy model to explore the heat diffusion within the heat-accumulating layer, and we test this model using numerical simulations. We formulate some generic features of the heat propagation which can be useful, for instance, for the interpretation of superbursts in accreting neutron stars. We present a self-similar analysis of late afterglow after such superbursts, which can be helpful to estimate properties of bursting stars.
