We present a linear mode analysis of the relativistic MHD equations in the presence of finite electrical conductivity. Starting from the fully relativistic covariant formulation, we derive the dispersion relation in the limit of small linear perturbations. It is found that the system supports ten wave modes which can be easily identified in the limits of small or large conductivities. In the resistive limit, matter and electromagnetic fields decouple and solution modes approach pairs of light and acoustic waves as well as a number of purely damped (non-propagating) modes. In the opposite (ideal) limit, the frozen-in condition applies and the modes of propagation coincide with a pair of fast magnetosonic, a pair of slow and Alfvén modes, as expected. In addition, the contact mode is always present and it is unaffected by the conductivity. For finite values of the conductivity, the dispersion relation gives rise to either pairs of opposite complex conjugate roots or purely imaginary (damped) modes. In all cases, the system is dissipative and also dispersive as the phase velocity depends nonlineary on the wavenumber. Occasionally, the group velocity may exceed the speed of light although this does not lead to superluminal signal propagation.
Comparison of magnetic diffusion and reconnection in ideal and resistive relativistic magnetohydrodynamics, ideal magnetodynamics, and resistive force-free electrodynamics
Resistive relativistic magnetohydrodynamics without Amperes Law
Institute for Theoretical Physics, University of Amsterdam（阿姆斯特丹大学理论物理研究所）；Dutch Institute for Emergent Phenomena（荷兰涌现现象研究所）；Institute for Advanced Study, University of Amsterdam（阿姆斯特丹大学高等研究院）；Niels Bohr International Academy, The Niels Bohr Institute, University of Copenhagen（哥本哈根大学尼尔斯·玻尔研究所尼尔斯·玻尔国际学院）；Anton Pannekoek Institute（安东·范内纽克研究所）
General-relativistic resistive-magnetohydrodynamics simulations of self-consistent magnetized rotating neutron stars
University of New Hampshire（新罕布什尔大学）；Los Alamos National Laboratory（洛斯阿拉莫斯国家实验室）；University of California, Berkeley（加州大学伯克利分校）；University of Illinois Urbana-Champaign（伊利诺伊大学厄巴纳-香槟分校）；National Center for Supercomputing Applications, University of Illinois Urbana-Champaign（伊利诺伊大学厄巴纳-香槟分校超级计算应用国家中心）；Academy of Athens（雅典科学院）；Universitat de Valéncia（瓦伦西亚大学）；Niels Bohr International Academy, Niels Bohr Institute（尼尔斯·玻尔国际学院，尼尔斯·玻尔研究所）；The Chinese University of Hong Kong（香港中文大学）；University of the Ryukyus（冲绳大学）
Extending the infrastructure of the BAM code towards resistive general-relativistic magnetohydrodynamics: tests and first applications
Max Planck Institute for Gravitational Physics (Albert Einstein Institute)（马克斯·普朗克引力物理研究所（爱因斯坦研究所））；Institut für Physik und Astronomie, Universität Potsdam（波茨坦大学物理与天文学研究所）；Centro de Ciências Naturais e Humanas, Universidade Federal do ABC（ABC联邦大学自然与人文科学中心）
Magnetic reconnection with a 0.1 rate: Effective resistivity in general relativistic magnetohydrodynamics
Canadian Institute for Theoretical Astrophysics（加拿大理论天体物理研究所）；Department of Physics, University of Toronto（多伦多大学物理系）；David A. Dunlap Department of Astronomy & Astrophysics, University of Toronto（多伦多大学大卫·邓拉普天文与天体物理系）；Perimeter Institute for Theoretical Physics（理论物理前沿研究所）；Department of Astronomy, Columbia University（哥伦比亚大学天文学系）；Center for Computational Astrophysics, Flatiron Institute（平顿研究所计算天体物理学中心）；Department of Physics, University of Maryland（马里兰大学物理系）；Princeton Center for Theoretical Science and Department of Astrophysical Sciences, Princeton University（普林斯顿大学理论科学中心和天体物理科学系）；Anton Pannekoek Institute（安东·潘内克研究所）
