强磁场与核意面相再研究
Strong magnetic fields and pasta phases revisited
AI总结：
本研究采用含表面项与库仑项的可压缩液滴模型，结合两种不同对称能斜率的相对论平均场模型，计算强磁场下中子星内壳结构，发现磁场致非均匀区延展依赖对称能，且旋节线不稳定性或源于外核密度涨落，该模型可更精准估算壳核转变参数与壳半径。
摘要：
在本研究中，我们计算了存在强磁场（如磁星中可观测到的强磁场）时中子星内壳的结构与组成。为确定壳层非均匀结构的几何形态与特征，我们采用可压缩液滴模型，将表面项与库仑项纳入变分方程，并将所得结果与基于更近似处理的既往计算结果进行对比。对于物态方程（EoS），我们选取两种具有不同对称能斜率的非线性相对论平均场模型开展研究，结果表明，磁场导致的恒星核心内部非均匀区域的延展程度，强烈依赖于壳层物态方程中对称能的行为特性。最后我们提出，既往计算中观测到的延展旋节线不稳定性，可能与磁星外核中存在的小振幅密度涨落相关，而非源于更厚的固体壳层。可压缩液滴模型的形式体系虽与既往计算总体一致，但会系统性地抑制亚稳解，从而能够更精确地估算壳-核转变密度与压强，进而更好地估算壳层半径。
英文摘要：
In this work, we compute the structure and composition of the inner crust of a neutron star in the presence of a strong magnetic field, such as it can be found in magnetars. To determine the geometry and characteristics of the crust inhomogeneities, we consider the compressible liquid drop model, where surface and Coulomb terms are included in the variational equations, and we compare our results with previous calculations based on more approximate treatments. For the equation of state (EoS), we consider two non-linear relativistic mean-field models with different slopes of the symmetry energy, and we show that the extension of the inhomogeneous region inside the star core due to the magnetic field strongly depends on the behavior of the symmetry energy in the crustal EoS. Finally, we argue that the extended spinodal instability observed in previous calculations can be related to the presence of small amplitude density fluctuations in the magnetar outer core, rather than to a thicker solid crust. The compressible liquid drop model formalism, while in overall agreement with the previous calculations, leads to a systematic suppression of the metastable solutions, thus allowing a more precise estimation of the crust-core transition density and pressure, and therefore a better estimation of the crustal radius.
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