Relativistic Radiative Flow in a Luminous Disk II

TL;DR

This paper investigates relativistic radiative flows above luminous disks, accounting for gravity, and demonstrates how flow velocity varies with luminosity and gravity effects, relevant to supercritical accretion disks.

Contribution

It introduces a method to solve relativistic radiative flow equations with a velocity-dependent Eddington factor, including gravity effects, extending previous models.

Findings

Flow reaches relativistic speeds in high luminosity cases.

Gravity reduces flow velocity in less luminous or smaller initial radius cases.

Application to supercritical accretion disks with mass loss is discussed.

Abstract

Radiatively-driven transfer flow perpendicular to a luminous disk is examined in the relativistic regime of $(v/c)^2$, taking into account the gravity of the central object. The flow is assumed to be vertical, and the gas pressure as well as the magnetic field are ignored. Using a velocity-dependent variable Eddington factor, we can solve the rigorous equations of the relativistic radiative flow accelerated up to the {\it relativistic} speed. For sufficiently luminous cases, the flow resembles the case without gravity. For less-luminous or small initial radius cases, however, the flow velocity decreases due to gravity. Application to a supercritical accretion disk with mass loss is briefly discussed.