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Relativistic radiative transfer and relativistic spherical shell flows

机译:相对论的辐射传递和相对论的球形壳流

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We examine a radiatively driven spherical flow from a central object, whose thickness is smaller than the radius of the central object, and a plane-parallel approximation can be used-a spherical shell flow. We first solve the relativistic radiative transfer equation iteratively, using a given velocity field, and obtain specific intensities as well as moment quantities. Using the obtained comoving flux, we then solve the relativistic hydrodynamical equation, and obtain a new velocity field. We repeat these double iteration processes until both the intensity and velocity profiles converge. We found that the flow speed v(tau) is roughly approximated as beta = v/c = beta(s)(1 - tau/tau(b)), where tau is the optical depth, tau(b) the flow total optical depth, and c the speed of light. We further found that the flow terminal speed v(s) is roughly expressed as beta(s) = v(s)/c = (Gamma (F) over cap (0) - 1)tau(b)/(m) over dot, where Gamma is the central luminosity normalized by the Eddington luminosity, (F) over cap (0) the comoving flux normalized by the incident flux, and of the order of unity, and (m) over dot the mass-loss rate normalized by the critical mass loss.
机译:我们检查了一个来自中心物体的辐射驱动的球面流,它的厚度小于中心物体的半径,并且可以使用平面平行近似-球壳流。我们首先使用给定的速度场迭代求解相对论的辐射传递方程,并获得比强度和矩量。然后使用获得的同运动通量,求解相对论流体力学方程,并获得新的速度场。我们重复这些双重迭代过程,直到强度和速度分布都收敛为止。我们发现流速v(tau)大致近似为beta = v / c = beta(s)(1- tau / tau(b)),其中tau是光学深度,tau(b)是总光学流速深度和c的光速。我们进一步发现流终端速度v(s)大致表示为beta(s)= v(s)/ c =(上限(0)-1时的gamma(F)-tau(b)/(m)以上点,其中Gamma是通过爱丁顿光度归一化的中心光度,(F)在上限(0)上通过入射通量归一化的同动通量,并且为单位数量级,并且(m)在点上的质量损失率归一化通过临界质量损失。

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