The Influence of Outflow in Supercritical Accretion Flows

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 asṀ ∝ 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 eff ∝ 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.

The influence of large-scale magnetic field in the structure of supercritical accretion flow with outflow

“…Our results reduce to the results of Zahra Zeraatgari et al (2016) without large scale magnetic field.…”

“…Also we ignore the relativistic effects and selfgravity of the disc and we use Newtonian gravity in the radial direction. We consider the effect of Bϕ,z on the dynamics of disc by following the paper of Zahra Zeraatgari et al (2016) in the presence of the effect of wind. Our results reproduce their solutions when the effect of large order magnetic field is neglected.…”

“…Furthermore the first self-similar solution for a magnetized ADAFs have been presented by Akizuki & Fukue (2006) which is able to reproduce general properties of slim discs. Zahra Zeraatgari et al (2016) studied the 1.5 dimensional self similar inflow-outflow equations of supercritical accretion flows with outflow in the absence of the magnetic field. They have followed the method of Bu et al (2009) and Xi & Yuan (2008) to study the effects of outflow by considering the interchange of mass, radial/angular momentum and energy between inflow and outflow.…”

Supercritical accretion of stellar-mass compact objects in active galactic nuclei

“…In inner parts where p rad > p gas and κ sct > κ abs , there exists a unique self-similar solution to the equations above with ṁin ∝ r, (Begelman 2012;Zahra Zeraatgari et al 2016. The self-similar solution in Newtonian gravity is consistent with numerical simulation results (Yuan et al 2012a,b;Sadowski et al 2014;McKinney et al 2014;Yang et al 2014;Takahashi et al 2018) for r 10m • .…”

“…is the torque that the part of disk with radius ≤ r exerts on the exterior part, with ν being the viscosity coefficient relating to the local sound speed c s and the disk height via ν = 2 3 αc s H following the commonly used α prescription (Shakura & Sunyaev 1973); η 1,2 measures the difference of the specific angular momentum (energy) carried by gas that turns around from inflow to outflow relative to that of gas still in the inflow at the same radius, and we take η 1 = η 2 = 0 considering that there should be no discontinuity between the two (see e.g., Xie & Yuan 2008;Zahra Zeraatgari et al 2016, for the impact of non-zero η 1,2 ).…”