Abstract
Relativistic radiative transfer in a relativistic spherical flow is examined in the fully special relativistic treatment. Under the assumption of a constant flow speed and using a variable (prescribed) Eddington factor, we analytically solve the relativistic moment equations in the comoving frame for several restricted cases, and obtain relativistic Milne-Eddington type solutions. In contrast to the plane-parallel case where the solutions exhibit the exponential behavior on the optical depth, the solutions have power-law forms. In the case of the radiative equilibrium, for example, the radiative flux has a power-law term multiplied by the exponential term. In the case of the local thermodynamic equilibrium with a uniform source function in the comoving frame, the radiative flux has a power-law form on the optical depth. This is because there is an expansion effect (curvature effect) in the spherical wind and the background density decreases as the radius increases.
Highlights
The research field of radiative transfer has been developed in astrophysics and atmospheric science [1,2,3,4,5,6,7,8,9,10,11,12,13]
Relativistic radiative transfer and relativistic radiation hydrodynamics have been developed in astrophysics and applied to various energetic phenomena in the universe: nova outbursts, gamma-ray bursts, astrophysical jets, black-hole accretion disks, and black-hole winds
We have examined the relativistic radiative transfer in the relativistic spherical flows in the fully special relativistic treatment
Summary
The research field of radiative transfer has been developed in astrophysics and atmospheric science [1,2,3,4,5,6,7,8,9,10,11,12,13]. Even in the subrelativistic regime, the FLD method cannot reproduce the radiative force precisely in the optically thin region [36]. The relativistic radiative transfer in relativistically moving atmospheres have been investigated from the analytical view points in the plane-parallel case (e.g., [37,38,39,40]) and in the spherical case (e.g., [41]). In Fukue [40], under the assumption of a constant flow speed, the relativistic moment equations in the comoving frame were analytically solved using a variable Eddington factor for several cases, such as the radiative equilibrium (RE) or the local thermodynamic equilibrium (LTE), and the relativistic Milne-Eddington type solutions for the relativistic plane-parallel flows have been newly found.
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