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Relativistic radiative transfer in a relativistic spherical flow is examined in the fully specialrelativistic 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 comovingframe 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 onthe 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 thecase of the local thermodynamic equilibrium with a uniform source function in the comovingframe, the radiative flux has a power-law form on the optical depth. This is because there is anexpansion effect (curvature effect) in the spherical wind and the background density decreasesas the radius increases

Relativistic Milne-Eddington Type Solutions with a Variable Eddington Factor for Relativistic Spherical Winds