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Relativistic radiative transfer in relativistic spherical flows

机译：相对论球形流动中的相对论辐射转移

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Relativistic radiative transfer in relativistic spherical flows is numerically examined under the fully special relativistic treatment. We first derive relativistic formal solutions for the relativistic radiative transfer equation in relativistic spherical flows. We then iteratively solve the relativistic radiative transfer equation, using an impact parameter method/tangent ray method, and obtain specific intensities in the inertial and comoving frames, as well as moment quantities, and the Eddington factor. We consider several cases; a scattering wind with a luminous central core, an isothermal wind without a core, a scattering accretion on to a luminous core, and an adiabatic accretion on to a dark core. In the typical wind case with a luminous core, the emergent intensity is enhanced at the center due to the Doppler boost, while it reduces at the outskirts due to the transverse Doppler effect. In contrast to the plane-parallel case, the behavior of the Eddington factor is rather complicated in each case, since the Eddington factor depends on the optical depth, the flow velocity, and other parameters.
机译：在完全特殊的相对论处理下，对相对论球流中的相对论辐射传输进行了数值研究。我们首先推导了相对论球流中相对论辐射传输方程的相对论形式解。然后，我们使用碰撞参数法/切线射线法迭代求解相对论辐射传输方程，并获得惯性系和共动系中的比强度、矩量和艾丁顿因子。我们考虑几种情况；有发光中心核心的散射风，没有核心的等温风，发光核心上的散射吸积，以及暗核心上的绝热吸积。在具有发光核心的典型风况下，由于多普勒增强，中心的出射强度增强，而在郊区由于横向多普勒效应，出射强度降低。与平面平行情况相比，在每种情况下，Eddington因子的行为都相当复杂，因为Eddington因子取决于光学深度、流速和其他参数。

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