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Black-Hole Winds with a Variable Eddington Factor

机译：爱丁顿因子可变的黑洞风

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We solve one-dimentinal spherically symmetric, optically thick black-hole winds under general relativity with the help of a variable Eddington factor, f (τ, β), where r is the optical depth and _ is the flow velocity normalized by the speed of light. Relativistic radiation hydrodynamics under the moment formalism has several complex prob_lems, such as a closure relation. Conventional relativistic moment equations closed with the traditional Eddington approximation in the comoving frame have a singularity, beyond which the flow cannot be accelerated. In order to avoid such a pathological behavior inherent in the relativistic moment formalism, we use a variable Eddington factor that depends on the flow velocity as well as the optical depth, for the case of spherically symmetric flow. We find luminous winds that can be accelerated by radiation pressure from a close vicinity to a black hole up to nearly the speed of light in a general-relativistic gravitational field.
机译：我们借助可变的爱丁顿因子f（τ，β）在广义相对论下求解一维球面对称，光学上较厚的黑洞风，其中r为光学深度，_为通过速度归一化的流速光。形式主义下的相对论辐射流体力学具有几个复杂的问题，例如封闭关系。在同动框架中用传统的Eddington逼近封闭的传统相对论矩方程具有奇异性，超过该奇异性将无法加速流动。为了避免相对论矩形式主义中固有的这种病理学行为，对于球形对称流，我们使用取决于流速以及光学深度的可变爱丁顿因子。我们发现，在广义相对论引力场中，可以通过辐射压力从近处到黑洞加速发光的风，其速度几乎达到光速。

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