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Paper   IPM / Astronomy / 12905
School of Astronomy
  Title:   Hydrodynamical wind in magnetized accretion flows with convection
1.  S. Abbassi
2.  A. Mosallanezhad
  Status:   Published
  Journal: Research in Astron. Astrophys.
  Vol.:  12
  Year:  2012
  Pages:   1625-1636
  Supported by:  IPM
The existence of outflow and magnetic field in the inner region of hot accretion flows have been confirmed by observations and numerical magnetohydrodynamic simulations (MHD). We present self-similar solutions for radiation inefficiently accretion flows (RIAF) around black holes in the presence of outflow and global magnetic field. The influence of outflow is taken into account by adopting a radius dependent of mass accretion rate · M = · M0(r/r0)s with s > 0 . Also we consider convection through a mixing length formalism to calculate convection parameter αcon . Moreover we consider the additional magnetic field parameters βr,φ,z[ = c2r,φ,z/(2 c2s) ] , where c2r,φ,z are the Alfvén sound speeds in three direction of cylindrical coordinate. Our numerical results show that by increasing all components of magnetic field, the surface density and rotational velocity increase although the sound speed and radial infall velocity of the disc decrease. Also we have found out 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 disc will increase when outflow becomes important in the radiation inefficiently accretion flow.

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