中子星表面层的偏振辐射传输
Polarized Radiation Transfer in Neutron Star Surface Layers
摘要：
研究中子星表面强磁化区域的偏振辐射传输对于理解吸积X射线双星、旋转动力双星和磁星具有重要意义。本文探讨了散射输运的经典磁汤姆逊域是广泛适用于这些中子星类。详细介绍了极化辐射转移的蒙特卡罗模拟的发展：它采用了电场矢量形式主义，使有关的线性，圆形和椭圆偏振的效用的广度。该模拟可适用于任何中子星表面，并适用于吸积柱和磁层问题。验证的代码强度和斯托克斯参数的确定说明了各种方式。从表面层的出射偏振信号的代表性结果提出了极地和赤道磁区，表现出对比两个区域之间的签名。这些特性还强烈依赖于光子频率与回旋频率的比率。高不透明度域的偏振签名，突出紧凑的解析近似的斯托克斯参数和各向异性相对于局部场方向的扩展范围内的频率。这些是非常有用的定义注入条件深的模拟板几何形状，加快从高度不透明的恒星大气的发射信号的产生。结果被解释在整个使用的磁汤姆逊微分截面的偏振特性。
英文摘要：
The study of polarized radiation transfer in the highly-magnetized surface locales of neutron stars is of great interest to the understanding of accreting X-ray pulsars, rotation-powered pulsars and magnetars. This paper explores scattering transport in the classical magnetic Thomson domain that is of broad applicability to these neutron star classes. The development of a Monte Carlo simulation for the polarized radiative transfer is detailed: it employs an electric field vector formalism to enable a breadth of utility in relating linear, circular and elliptical polarizations. The simulation can be applied to any neutron star surface locale, and is adaptable to accretion column and magnetospheric problems. Validation of the code for both intensity and Stokes parameter determination is illustrated in a variety of ways. Representative results for emergent polarization signals from surface layers are presented for both polar and equatorial magnetic locales, exhibiting contrasting signatures between the two regions. There is also a strong dependence of these characteristics on the ratio of the frequency of a photon to the cyclotron frequency. Polarization signatures for high opacity domains are presented, highlighting compact analytic approximations for the Stokes parameters and anisotropy relative to the local field direction for an extended range of frequencies. These are very useful in defining injection conditions deep in the simulation slab geometries, expediting the generation of emission signals from highly opaque stellar atmospheres. The results are interpreted throughout using the polarization characteristics of the magnetic Thomson differential cross section.
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