Electrical conductivity of a warm neutron star crust in magnetic fields
Electrical conductivity of a warm neutron star crust in magnetic fields
复制标题
磁场中温暖中子星地壳的电导率
DOI：
--
复制
发表时间：
2016
期刊：
影响因子：
--
通讯作者：
A. Sedrakian
中科院分区：
文献类型：
--
作者：
A. Harutyunyan;A. Sedrakian
我们研究了一个温暖的致密星星的有限温度地壳的电导率，它可能是在超新星爆炸或双星中子星星合并以及当一个冷的中子星星被从伴星吸积的材料加热后形成的。我们专注于等离子体是在液体状态的温度-密度制度，因此，电导率是由相关核的电子散射为主。这种相互作用的动力学屏蔽是根据QED等离子体硬热环有效场理论中计算的极化张量实现的。背景离子成分的相关性占通过来自单组分等离子体的Monte Carlo模拟的结构因子。有了这个输入，我们解决了玻尔兹曼动力学方程的弛豫时间近似考虑到各向异性的运输，由于磁场。电导率张量的数值研究作为一个函数的温度和密度的碳和铁的核，以及密度依赖于零温致密物质的组成与电子处于弱平衡。我们还提供了精确的拟合公式，我们的数值结果，以及补充表，可用于耗散的热致密星的磁流体动力学模拟。
We study the electrical conductivity of finite-temperature crust of a warm compact star which may be formed in the aftermath of a supernova explosion or a binary neutron star merger as well as when a cold neutron star is heated by accretion of material from a companion. We focus on the temperature-density regime where plasma is in the liquid state and, therefore, the conductivity is dominated by the electron scattering off correlated nuclei. The dynamical screening of this interaction is implemented in terms of the polarization tensor computed in the hard-thermal-loop effective field theory of QED plasma. The correlations of the background ionic component are accounted for via a structure factor derived from Monte Carlo simulations of one-component plasma. With this input we solve the Boltzmann kinetic equation in relaxation time approximation taking into account the anisotropy of transport due to the magnetic field. The electrical conductivity tensor is studied numerically as a function of temperature and density for carbon and iron nuclei as well as density-dependent composition of zero-temperature dense matter in weak equilibrium with electrons. We also provide accurate fit formulas to our numerical results as well as supplemental tables which can be used in dissipative magneto-hydrodynamics simulations of warm compact stars.