Relativistic radiative shocks in disk accretion
Relativistic radiative shocks in disk accretion
复制标题
盘吸积中的相对论辐射冲击
DOI：
10.1093/mnras/sty3380
复制
发表时间：
2019
期刊：
影响因子：
--
通讯作者：
Jun Fukue
中科院分区：
文献类型：
--
作者：
長谷川賢二;Jun Fukue
相对论辐射激波，这是稳定地站在相对论盘吸积流，检查下的平衡扩散近似和爱丁顿之一，在光学厚的制度，考虑到垂直流体静力平衡。与非相对论情况类似，表面密度表现得像通常激波中的气体密度，并且在辐射压力主导的激波中增加到7，尽管激波后区域中的气体密度由于激波前沿后面的垂直膨胀而经常降低。因此，在冲击波后区域，垂直方向的光学厚度增加，而径向的光学厚度减小。与通常的辐射激波和非相对论情况类似，在激波阵面前的预激波区，出现了辐射前兆，由于辐射扩散效应，辐射能量衰减到预激波区。对于气体和辐射压力主导的情况，我们导出了相对论圆盘吸积流中相对论辐射激波的整体跳跃条件，并以跳跃条件为边界条件求解了辐射前兆的激波结构。这些解是相对论性盘吸积激波问题的基本解，需要从多方面加以发展。
Relativistic radiative shock waves, which are steadily standing in relativistic disc accretion flows, are examined under the equilibrium diffusion approximation and the Eddington one in the optically thick regime, taking into account the vertically hydrostatic equilibrium. Similar to the non-relativistic case, the surface density behaves like the gas density in the usual shocks, and increases up to 7 in the radiation-pressure-dominated shock, although the gas density in the post-shock region often decreases due to the vertical expansion behind the shock front. Hence, the optical depth in the vertical direction rises up in the post-shock region, while that in the radial direction reduces. Similar to the usual radiative shock and non-relativistic case, in the pre-shock region before the shock front, there appears a radiative precursor, where the radiation energy attenuates into the pre-shock region due to the radiative diffusion effect. For both the gas and radiation-pressure-dominated cases, we derive the overall jump conditions for the relativistic radiative shock in relativistic disc accretion flows, and solve the shock structure of the radiative precursor with jump conditions as boundary conditions. The solutions are quite fundamentals in relativistic disc accretion shock problems around a compact object, and should be developed in various aspects.