中子星壳层旋转破裂中的冻结组分效应
Frozen-composition effects on rotational failure of neutron-star crusts
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中文总结 AI 辅助
本研究利用统一状态方程比较化学平衡与冻结组分下中子星壳层旋转破裂，发现冻结组分降低破裂频率（BSk24降21.7%）并改变破裂位置，揭示化学非平衡对破裂阈值和起始层的显著影响。
中文摘要 AI 辅助
中子星壳层对旋转加载的弹性响应取决于形变过程中弱相互作用能否恢复化学平衡。我们利用统一状态方程量化了这一效应，并在相同的牛顿流体-弹性框架内比较了化学平衡与冻结组分响应。冻结组分增加了有效体积模量，并在内壳层中重新分布应变，而非产生简单的整体重新标度。对于BSk24，破裂频率从$0.4997\Omega_K$降至$0.3912\Omega_K$，降低了21.7%，且首次破裂位置移至更高密度。BSk21获得了相当的降幅，而SLy4的效应较小，为16.7%。对于BSk24，在$1.2$--$2.0,M_\odot$质量范围内，相对降幅保持在21--22%附近。密度分辨的微扰分析表明，该结果由微观冻结组分硬化与壳层力学敏感性之间的径向重叠控制，BSk模型中大部分线性敏感性来自$0.01<n_B<0.03,{\rm fm}^{-3}$。这些结果表明，化学非平衡可显著改变旋转破裂阈值及壳层破裂起始层。
英文摘要
The elastic response of a neutron-star crust to rotational loading depends on whether weak interactions can restore chemical equilibrium during the deformation. We quantify this effect using unified equations of state and compare chemically equilibrated and frozen-composition responses within the same Newtonian hydro-elastic framework. Frozen composition increases the effective bulk modulus and redistributes the strain throughout the inner crust rather than producing a simple global rescaling. For BSk24, the breaking frequency decreases from $0.4997Ω_K$ to $0.3912Ω_K$, a reduction of 21.7 per cent, while the location of first failure moves to higher density. Comparable reductions are obtained for BSk21, whereas SLy4 gives a smaller effect of 16.7 per cent. For BSk24 the relative reduction remains close to 21--22 per cent over the mass range $1.2$--$2.0,M_\odot$. A density-resolved perturbation analysis shows that the result is controlled by the radial overlap between the microphysical frozen-composition stiffening and the mechanical susceptibility of the crust, with most of the linear sensitivity in the BSk models arising from $0.01<n_B<0.03,{\rm fm}^{-3}$. These results show that chemical non-equilibrium can substantially modify both the rotational failure threshold and the layer in which crustal failure begins.
