康普顿散射是热中子星、黑洞周围的吸积盘和热日冕中的主要不透明度源。本文收集了一组非偏振辐射（RF）康普顿散射再分布函数的数值表达式，它比广泛使用的Kompaneets方程更精确。本文的主要目的是介绍Guilbert（1981）的RF，并对原始论文中的计算错误进行了修正。这一修正的RF被用于热中子星大气模型计算的系列论文中。我们还组织了四个现有的算法的RF计算成一个统一的形式，准备在辐射转移和模式大气代码中使用。Nagirner和Poutanen（1993）的精确方法在从硬X射线到无线电波的非常宽的光谱范围内与所有其他算法进行了数值比较。对对应于爆发中子星大气和热星系际介质温度的热等离子体中康普顿散射再分布函数进行了抽样计算。我们的公式也适用于研究非极化微波背景辐射在热团簇内气体中的康普顿散射和Sunyaev-Zeldovich效应。我们的结论是，Guilbert（1981）的公式和精确的量子力学公式实际上给出了与X射线爆发中子星大气层相关的气体温度的再分布函数$T \le 10^8$ K.
英文摘要：
Compton scattering is the dominant opacity source in hot neutron stars, accretion disks around black holes and hot coronae. We collected here a set of numerical expressions of the Compton scattering redistribution functions for unpolarized radiation (RF), which are more exact than the widely used Kompaneets equation. The principal aim of this paper is presentation of the RF by Guilbert (1981) which is corrected for the computational errors in the original paper. This corrected RF was used in the series of papers on model atmosphere computations of hot neutron stars. We have also organized four existing algorithms for the RF computations into a unified form ready to use in radiative transfer and model atmosphere codes. The exact method by Nagirner and Poutanen (1993) was numerically compared to all other algorithms in a very wide spectral range from hard X-rays to radio waves. Sample computations of the Compton scattering redistribution functions in thermal plasma were done for temperatures corresponding to the atmospheres of bursting neutron stars and hot intergalactic medium. Our formulae are also useful to the study Compton scattering of unpolarised microwave background radiation in hot intra-cluster gas and the Sunyaev-Zeldovich effect. We conclude, that the formulae by Guilbert (1981) and the exact quantum mechanical formulae yield practically the same redistribution functions for gas temperatures relevant to the atmospheres of X-ray bursting neutron stars, $T \le 10^8$ K.
Fingerprints of thermal Comptonization in accreting neutron stars. Plasma-vacuum interplay in cyclotron lines and polarisation
Dr. Karl Remeis-Observatory and Erlangen Centre for Astroparticle Physics, Friedrich-Alexander Universität Erlangen-Nürnberg（弗里德里希-亚历山大埃尔朗根-纽伦堡大学卡尔·雷梅斯天文台和埃尔朗根天体粒子物理中心）；INAF - IASF Palermo（意大利国家天体物理研究所巴勒莫分院）；Dipartimento di Fisica e Chimica Emilio Segrè, Università degli Studi di Palermo（巴勒莫大学埃米利奥·塞格雷物理与化学系）；Department of Astronomy, University of Geneva（日内瓦大学天文学系）；INAF, Osservatorio Astronomico di Brera（意大利国家天体物理研究所布里拉天文台）；School of Physics and Astronomy, University of Southampton（南安普顿大学物理与天文学学院）
One-dimensional PIC Simulation of Induced Compton Scattering in Magnetized Electron-Positron Pair Plasma
Center for Gravitational Physics and Quantum Information, Yukawa Institute for Theoretical Physics, Kyoto University（京都大学汤川理论物理研究所引力物理与量子信息中心）；Department of Physics, Kyoto University（京都大学物理学系）；Graduate School of System Informatics, Kobe University（神户大学系统信息学研究）
The Cosmological Impact of Luminous TeV Blazars I: Implications of Plasma Instabilities for the Intergalactic Magnetic Field and Extragalactic Gamma-Ray Background
Impact of Resonant Compton Scattering on Magnetar X-Ray Polarization with QED Vacuum Resonance
School of Physics and Astronomy, Shanghai Jiao Tong University（上海交通大学物理与天文学院）；Tsung-Dao Lee Institute, Shanghai Jiao Tong University（上海交大李政道研究所）；Center for Astrophysics and Planetary Science, Department of Astronomy, Cornell University（康奈尔大学天文学系天体物理学与行星科学中心）
