Magnetic fields play an important role in creating, driving, and in the evolution of outflows and jets from protostars and accretion disks. On the other hand, the temperature profile of the accretion disks may also affect the structure of the magnetic field and outflows. In this paper, we use the self-similar method in cylindrical coordinates to investigate the effect of the temperature profile...

in this work we solve the set of hydrodynamical equations for accretion disks in the spherical coordinates (r,θ,ϕ) to obtain the explicit structure along θ direction. we study a two-dimensional advective accretion disc in the presence of thermal conduction. we find self-similar solutions for an axisymmetric, rotating, steady, viscous-resistive disk. we show that the global structure of an advec...

magnetic fields play an important role in creating, driving, and in the evolution of outflows and jets from protostars and accretion disks. on the other hand, the temperature profile of the accretion disks may also affect the structure of the magnetic field and outflows. in this paper, we use the self-similar method in cylindrical coordinates to investigate the effect of the temperature profile...

In this work we solve the set of hydrodynamical equations for accretion disks in the spherical coordinates (r,θ,ϕ) to obtain the explicit structure along θ direction. We study a two-dimensional advective accretion disc in the presence of thermal conduction. We find self-similar solutions for an axisymmetric, rotating, steady, viscous-resistive disk. We show that the global structure of an advec...

Accretion disk theory was first developed as a theory with the local heat balance, where the whole energy produced by a viscous heating was emitted to the sides of the disk. One of the most important new invention of this theory was the phenomenological treatment of the turbulent viscosity , known the " alpha " prescription, where the (rφ) component of the stress tensor was approximated by (αp)...

Young stellar systems orbiting in the potential of their birth cluster can accrete from the dense molecular interstellar medium during the period between the star’s birth and the dispersal of the cluster’s gas. Over this time, which may span several Myr, the amount of material accreted can rival the amount in the initial protoplanetary disk; the potential importance of this ‘tail-end’ accretion...