The influence of outflow in supercritical accretion flows

TL;DR

This paper investigates how outflows affect supercritical accretion flows by solving radiation-hydrodynamic equations with self-similar solutions, revealing key temperature profiles and the impact of outflows on flow dynamics and luminosity.

Contribution

It introduces a power-law model for mass inflow rate in supercritical accretion flows and analyzes the effects of outflows on flow structure and emitted spectra.

Findings

Effective temperature scales as r^{-1/2} with radius.

Outflows significantly influence accretion flow dynamics.

The advection parameter f depends strongly on mass inflow rate.

Abstract

We solve the radiation-hydrodynamic (RHD) equations of supercritical accretion flows in the presence of radiation force and outflow by using self similar solutions. Compare with the pioneer works, in this paper we consider power-law function for mass inflow rate as $ \dot{M} \propto r^{s} $. We found that $ s = 1 $ when the radiative cooling term is included in the energy equation. Correspondingly, the effective temperature profile with respect to the radius was obtained as $ T_{\text{eff}} \varpropto r^{-1/2} $. In addition, we investigated the influence of the outflow on the dynamics of the accretion flow. We also calculated the continuum spectrum emitted from the disk surface as well as the bolometric luminosity of the accretion flow. Furthermore, our results show that the advection parameter, $ f $, strongly depends on mass inflow rate.