Numerical simulation of X-ray-heated winds in Seyfert galaxies. I - The case of zero angular momentum
Numerical simulation of X-ray-heated winds in Seyfert galaxies. I - The case of zero angular momentum
复制标题
塞弗特星系中 X 射线加热风的数值模拟。
DOI：
10.1086/172116
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发表时间：
1993
期刊：
影响因子：
--
通讯作者：
J. Krolik
中科院分区：
文献类型：
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作者：
D. Balsara;J. Krolik
数值流体动力学模拟显示了 X 射线加热的风，这些风被认为形成了“镜子”，将来自模糊的塞弗特星系核的光反射到我们的视线中。在可能的参数范围之上，表明当冷环面围绕活动星系核时会产生稳态流。从环面内边缘蒸发的一些质量被中央引力井捕获，而其余的则被温暖的风吹走。当中心重力相对于辐射加热速率较强时，即L/L(E)较小时，几乎所有注入的物质都被捕获。当重力较弱时，给定的加热速率和注入压力组合会导致最大质量损失率；当质量注入的速率超过该量时，多余的部分将被捕获。这两种情况之间的分界线为 L/L(E) = 约 0.08。
Numerical hydrodynamics simulations are presented of X-ray heated winds believed to form the 'mirrors' which reflect light from obscured Seyfert galaxy nuclei into our line of sight. Above a likely range of parameters, it is shown that steady state flows are created when a cool torus surrounds an AGN. Some of the mass evaporated off the inner edge of the torus is captured by the central gravitational well, while the rest is driven off in a warm wind. When the central gravity is strong relative to the radiative heating rate, i.e., L/L(E) is small, nearly all the injected matter is captured. When the gravity is weaker, a given combination of heating rate and injected pressure leads to a maximum mass loss rate; when the rate at which mass is injected exceeds this amount, the excess is captured. The dividing line between these two cases comes at L/L(E) = about 0.08.