Radiative Flow in a Luminous Disk II

Abstract

Radiatively-driven transfer flow perpendicular to a luminous disk is examined in the subrelativistic regime of (v/c) 1 , taking into account the gravity of the central object. The flow is assumed to be vertical, and the gas pressure is ignored, while internal heating is assumed to be proportional to the gas density. The basic equations were numerically solved as a function of the optical depth, and the flow velocity, the height, the radiative flux, and the radiation pressure were obtained for a given radius, an initial optical depth, and initial conditions at the flow base (disk "inside"), whereas the mass-loss rate was determined as an eigenvalue of the boundary condition at the flow top (disk "surface"). For sufficiently luminous cases, the flow resembles the case without gravity. For less-luminous cases, however, the flow velocity decreases, and the flow would be impossible due to the existence of gravity in the case that the radiative flux is sufficiently small. Application to a supercritical accretion disk with mass loss is briefly discussed.

Relativistic Radiative Flow in a Luminous Disk II

“…Second, on contrary to the final speed, the mass-loss rate per unit area increases as the initial radius decreases; it is roughly approximated by J ∼ 6/r. On the other hand, the model mass-loss rate (Fukue 2004(Fukue , 2006a becomes J = 1/r, that is qualitatively same, but quantitatively different from the present numerical values. Hence, the mass loss from the critical disk may be concentrated in the inner region, although the true mass-loss rate cannot be determined at the present simple state.…”

“…Recently, mass outflow as well as radiation transfer have been examined for the first time in the subrelativistic (Fukue 2005a(Fukue , 2006a and fully relativistic cases (Fukue 2005b). In the latter case, it is pointed out some singular behavior inherent in the relativistic radiative flow (e.g., Turolla, Nobili 1988;Turolla et al 1995;Dullemond 1999).…”

Radiative Transfer in Relativistic Accretion-Disk Winds

“…In these earlier works, however, the radiation fields are set to be external sources, and the radiation transfer was not considered. Recently, radiative transfer in a moving disk atmosphere was firstly investigated in the subrelativistic regime (Fukue 2005a(Fukue , 2006a, and in the relativistic regime (Fukue 2005b(Fukue , 2006bFukue, Akizuki 2006b). In these studies, however, only the radiative moments were obtained under the moment formalism, and the specific intensity was not solved.…”

Radiative Transfer in Accretion-Disk Winds

“…In this paper, we thus examine radiative transfer in the accretion disk wind, which is assumed to blow off from the luminous disk in the vertical direction (planeparallel approximation), and analytically and numerically obtain the flow solutions for the case without internal heating. In the previous studies, radiative flows in the vertically moving atmosphere were solved in the subrelativistic regime (Fukue 2005a(Fukue , 2006a, and in the relativistic regime (Fukue 2005b(Fukue , 2006bFukue, Akizuki 2006b), where only radiative moments were obtained. In the present paper, we further obtain the radiation intensity as well as radiative moments.…”

“…Radiative transfer in the accretion disk wind, on the other hand, has not been well considered both in the nonrelativistic and relativistic regimes. Recently, radiative transfer in a moving disk atmosphere was firstly investigated in the subrelativistic regime (Fukue 2005a(Fukue , 2006a, and in the relativistic regime (Fukue 2005b(Fukue , 2006bFukue, Akizuki 2006b). In contrast to the static atmosphere, in the moving atmosphere the boundary condition at the surface of zero optical depth should be modified (Fukue 2005a, b).…”