Radiatively-suppressed spherical accretion under relativistic radiative transfer

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Abstract

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We numerically examine radiatively-suppressed relativistic spherical accretion flows on to a central object with mass M under Newtonian gravity and special relativity. We simultaneously solve both the relativistic radiative transfer equation and the relativistic hydrodynamical equations for spherically symmetric flows under the double iteration process in the case of the intermediate optical depth. We find that the accretion flow is suppressed, compared with the freefall case in the nonrelativistic regime. For example, in the case of accretion on to a luminous core with accretion luminosity L*, the freefall velocity v normalized by the speed of light c under the radiative force in the nonrelativistic regime is β(r^)=v/c=-(1-Γ〓)/(r^+1-Γ〓)-----------------√⁠, where Γ* (≡ L*/LE, LE being the Eddington luminosity) is the Eddington parameter and r^ (= r/rS, rS being the Schwarzschild radius) the normalized radius, whereas the infall speed at the central core is 〓0.7β(1), irrespective of the mass-accretion rate. This is due to the relativistic effect; the comoving flux is enhanced by the advective flux. We briefly examine and discuss an isothermal case, where the emission takes place in the entire space.

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