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

## TL;DR

This paper investigates how large-scale magnetic fields influence the structure and dynamics of supercritical accretion flows with outflows, revealing that magnetic components significantly affect disc thickness, velocities, temperature, and luminosity.

## Contribution

It introduces a self-similar, 1.5D model of magnetized supercritical accretion flows with outflows, analyzing the effects of magnetic field components on flow structure and properties.

## Key findings

- Toroidal magnetic field increases disc thickness and velocities.
- Vertical magnetic field decreases disc thickness.
- Luminosity remains constant for high accretion rates.

## Abstract

We present the effects of ordered large scale magnetic field on the structure of supercritical accretion flow in the presence of outflow. In the cylindrical coordinates ($r, \varphi,z$), We write the 1.5 dimensional, the steady state ($\frac{\partial}{\partial t}=0$) and axisymmetric ($\frac{\partial}{\partial \varphi}=0$) inflow-outflow equations by using the self similar solutions. Also a model for radiation pressure supported accretion flow threaded by both toroidal and vertical components of magnetic field has been formulated. For studying the outflows, we adopt a radius dependent mass accretion rate as $\dot{M}=\dot{M}_{out}{(\frac{r}{r_{out}})^{s+\frac{1}{2}}}$ with $s=\frac{1}{2}$. Also by following the previous works, we have considered the interchange of mass, radial and angular momentum and the energy between inflow and outflow. we have found numerically that two components of magnetic field have the opposite effects on the thickness of the disc and similar effects on the radial and angular velocities of the flow. We have found that the existence of the toroidal component of magnetic field will lead to increasing of radial and azimuthal velocities as well as the relative thickness of the disc, which is increased . Moreover, the thickness of the disc will decrease when the vertical component of magnetic field becomes important in magnetized flow. The solutions indicated that the mass inflow rate, the specific energy of outflow affect strongly on the advection parameter.We have shown that by increasing the two components of magnetic field, the temperature of the accretion flow will decrease significantly. On the other hand we have shown the bolometric luminosity of the slim discs for high values of $\dot{m} (\dot{m}>>1)$ is not sensitive to mass accretion rate and is kept constant ($L \approx 10 L_{E}$).