Hydrodynamical wind in magnetized accretion flows with convection

作     者：Shahram Abbassi Amin Mosallanezhad 

作者机构：School of PhysicsDamghan UniversityP.O.Box 36715-364DamghanIran School of AstronomyInstitute for Research in Fundamental SciencesP.O.Box 19395-5531 TehranIran Center for Excellence in Astronomy&Astrophysics(CEAA-RIAAM)P.O.Box 55134-441 MaraghaIran 

出 版 物：《Research in Astronomy and Astrophysics》 (天文和天体物理学研究（英文版）)

年 卷 期：2012年第12卷第12期

页      面：1625-1636页

核心收录：

学科分类：07[理学] 070401[理学-天体物理] 0704[理学-天文学] 

主　　题：accretion:accretion flow wind:outflow convection:MHD 

摘      要：The existence of outflow and magnetic fields in the inner region of hot accretion flows has been confirmed by observations and numerical magnetohydrodynamic（MHD）*** present self-similar solutions for radiatively inefficient accretion flows（RIAFs）around black holes in the presence of outflow and a global magnetic *** influence of outflow is taken into account by adopting a radius that depends on mass accretion rateM=M0 （r/r0）s with s〉0. We also consider convection through a mixing length formula to calculate convection parameterα*** we consider the additional magnetic field parameters βr,φ,z=c2 r,φ,z /（2c2 s ）,where c2 r,φ,z are the Alfvén sound speeds in three directions of cylindrical *** 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 *** have also found that the existence of wind will lead to reduction of surface density as well as rotational ***,the radial velocity,sound speed,advection parameter and the vertical thickness of the disk will increase when outflow becomes important in the RIAF.