论文标题
吸收中子星：内皮的上层加热
Accreting neutron stars: heating of the upper layers of the inner crust
论文作者
论文摘要
低质量X射线二进制中的中子恒星被认为是由壳中的放热核反应加热的。能量释放和加热源的位置是热演化模型的重要成分。在这里，我们介绍了恒星外壳三个区域中能量释放的热力学一致的计算：在外壳的外壳界面，内部地壳的上层（最多可密度$ρ\ leq 2 \ leq 2 \ times 10^{12} $ g cm $ $ $ g cm $^{ - 3} $），以及在下面的colustal colustal层中。我们考虑了三种代表性的热核灰分模型（Superburst，Extreme RP和Kepler Ashes）。每个区域中的能量释放是通过外壳界面处的压力来参数化的，外壳界面的压力编码了与最深内膜最深的物理学相关的所有不确定性。我们的计算尤其使我们能够对净能量释放（每块baryon）设置新的下限：$ q \ gtrsim0.28 $ MEV用于极端RP灰烬，Q〜0.43-0.51 MEV用于Superburst和Kepler Ashes。
Neutron stars in low-mass X-ray binaries are thought to be heated up by accretion-induced exothermic nuclear reactions in the crust. The energy release and the location of the heating sources are important ingredients of the thermal evolution models. Here we present thermodynamically consistent calculations of the energy release in three zones of the stellar crust: at the outer-inner crust interface, in the upper layers of the inner crust (up to the density $ρ\leq 2\times 10^{12}$ g cm$^{-3}$), and in the underlying crustal layers. We consider three representative models of thermonuclear ashes (Superburst, Extreme rp, and Kepler ashes). The energy release in each zone is parametrized by the pressure at the outer-inner crust interface, which encodes all uncertainties related to the physics of the deepest inner-crust layers. Our calculations allow us, in particular, to set new lower limits on the net energy release (per accreted baryon): $Q\gtrsim0.28$ MeV for Extreme rp ashes and Q~0.43-0.51 MeV for Superburst and Kepler ashes.
