Numerical simulation of hot accretion flows with thermal conduction

We report on the effects of isotropic thermal conduction in non-radiative collisionless accretion flows in two dimensions.In comparison to accretion flows without conduction,we find that the disk generally becomes cooler and thinner.Specifically,the magnitude of this effect depends on the kinetic viscosity coefficient.If it is proportional to density,the density profile of the accretion flow is flat,therefore the effect is not very obvious.But,if it is proportional to r1/2,as is usual for the "α" disk description,the density profile is steeper.Therefore,the effect will be much more obvious,with the temperature profile of the accretion flow becoming much flatter.This will have important observational consequences.