Stergioulas Nikolaos
Department of Physics, University of Wisconsin-Milwaukee, PO Box 413, Milwaukee, WI 53201 USA ; Max Planck Institute for Gravitational Physics (Albert-Einstein-Institute), D-14473 Potsdam, Germany.
Living Rev Relativ. 1998;1(1):8. doi: 10.12942/lrr-1998-8. Epub 1998 Jun 18.
Because of the information they can yield about the equation of state of matter at extremely high densities and because they are one of the more possible sources of detectable gravitational waves, rotating relativistic stars have been receiving significant attention in recent years. We review the latest theoretical and numerical methods for modeling rotating relativistic stars, including stars with a strong magnetic field and hot proto-neutron stars. We also review nonaxisymmetric oscillations and instabilities in rotating stars and summarize the latest developments regarding the gravitational wave-driven (CFS) instability in both polar and axial quasi-normal modes.
由于旋转相对论性恒星能够提供有关极高密度下物质状态方程的信息,并且它们是可探测引力波更有可能的来源之一,近年来受到了广泛关注。我们回顾了用于模拟旋转相对论性恒星的最新理论和数值方法,包括具有强磁场的恒星和热原中子星。我们还回顾了旋转恒星中的非轴对称振荡和不稳定性,并总结了极向和轴向准正则模中引力波驱动(CFS)不稳定性的最新进展。