The existence of outflow in accretion flows is confirmed by observations and magnetohydrodynamics (MHD) simulations. In this paper, we study outflows of accretion flows in the presence of resistivity and toroidal magnetic field. The mechanism of energy dissipation in the flow is assumed to be the viscosity and the magnetic diffusivity due to turbulence in the accretion flow. It is also assumed that the magnetic diffusivity and the kinematic viscosity are not constant and vary by position and $α$-prescription is used for them. The influence of outflow emanating from accretion disc is considered as a sink for mass, angular momentum and energy. The self-similar method is used to solve the integrated equations that govern the behavior of the accretion flow in the presence of outflow. The solutions represent the disc which rotates faster and becomes cooler for stronger outflows. Moreover, by adding the magnetic diffusivity, the surface density and rotational velocity decrease, while the radial velocity and temperature increase. The study of present model with the magnitude of magnetic field implies that the disc rotates and accretes faster and becomes hotter, while the surface density decreases. The disc thickness increases by adding the magnetic field or resistivity, while it becomes thinner for more losses of mass and energy due to the outflows.
Self-similar solutions of viscous and resistive ADAFs with thermal conduction
本文研究了热传导对粘性和阻力对流主导吸积流结构的影响。热传导对热吸积流的重要性被围绕着Sgr A $^*$和其他几个附近星系核的热气体的观测所证实。在本研究中，热传导是由它的饱和形式来研究的，因为它适合于弱碰撞系统。假设粘性和磁扩散率是由于流动中的湍流和耗散。粘性也是由于角动量传输。这里，磁扩散率和运动粘度不是恒定的，并且随位置而变化，并且$α$ -处方用于它们。用定常自相似方法求解了系统的控制方程。结果表明，径向速度是高度亚音速和旋转速度的行为亚开普勒。对于热传导系数的特定值，旋转速度变为零。该电导率的量强烈地依赖于磁压分数、磁普朗特数和粘度参数。通过热传导与其他能量机制的能量传输的比较表明，热传导可以是电阻和磁化ADAF中的重要能量机制。非理想磁流体动力学（MHD）模拟证实了这一属性。
A 2.5-dimensional viscous, resistive, advective magnetized accretion-outflow coupling in black hole systems: A higher order polynomial approximation. I
