A class of self-gravitating, magnetized accretion disks

Abstract

The steady-state structure of self-gravitating, magnetized accretion disks is studied using a set of self-similar solutions which are appropriate in the outer regions. The disk is assumed to be isothermal and the magnetic field outside of the disk is treated in a phenomenological way. However, the internal field is determined self-consistently. The behaviour of the solutions are investigated by changing the input parameters of the model, i.e. mass accretion rate, coefficients of viscosity and resistivity, and the magnetic field configuration.

Accepted by ApJ

References in corpus (7)

• The locality of transport in self-gravitating accretion discs
• Nonlinear Outcome of Gravitational Instability in Disks with Realistic Cooling
• Protostellar Disks: Formation, Fragmentation, and the Brown Dwarf Desert
• Fragmentation of a Molecular Cloud Core versus Fragmentation of the Massive Protoplanetary Disk in the Main Accretion Phase
• The effect of MHD turbulence on massive protoplanetary disk fragmentation
• A Model for Quasi-Spherical Magnetized Accretion Flow
• Self-similar structure of the magnetized radiation-dominated accretion disks

Cited by in corpus (8)

• Relating Kerr SMBHs in Active Galactic Nuclei to RAD configurations
• Self-similar structure of magnetized ADAFs and CDAFs
• Viscous accretion of a polytropic self-gravitating disk in the presence of wind
• Numerical study of self-gravitating protoplanetary discs
• Structure of ADAFs in a general large-Scale B-field: The role of wind and thermal conduction
• Hydrodynamical wind on magnetized Accretion Flows with Convection
• Self-Gravity in Magnetized Neutrino-Dominated Accretion Discs
• Dynamics of charged dust particles in protoplanetary discs