Hydrodynamical wind in magnetized accretion flows with convection

作者：Abbassi Shahram^*; Mosallanezhad Amin

来源：Research in Astronomy and Astrophysics, 2012, 12(12): 1625-1636.

DOI：10.1088/1674-4527/12/12/004

• accretion: accretion flow
• wind: outflow
• convection: MHD

The existence of outflow and magnetic fields in the inner region of hot accretion flows has been confirmed by observations and numerical magnetohydrodynamic (MHD) simulations. We present self-similar solutions for radiatively inefficient accretion flows (RIAFs) around black holes in the presence of outflow and a global magnetic field. The influence of outflow is taken into account by adopting la radius that depends on mass accretion rate (M) over dot = (M) over dot(0) (r/r(0))(s) with s > 0. We also consider convection through a mixing length formula to calculate convection parameter alpha(con). Moreover we consider the additional magnetic field parameters beta(r,phi, z)[ = c(r,phi,z)(2)/2c(s)(2))] , where c(r,phi,z)(2) are the Alfven sound speeds in three directions of cylindrical coordinates. Our numerical results show that by increasing all components of the magnetic field, the surface density and rotational velocity increase, but the sound speed and radial infall velocity of the disk decrease. We have also found that the existence of wind will lead to reduction of surface density as well as rotational velocity. Moreover, the radial velocity, sound speed, advection parameter and the vertical thickness of the disk will increase when outflow becomes important in the RIAF.

• 出版日期2012-12