Luminous hot accretion disks

We find a new two-temperature hot branch of equilibrium solutions for stationary accretion disks around black holes. In units of Eddington accretion rate defined as 10LEdd/c , the accretion rates to which these solutions correspond are within the range ṁ1 <∼ ṁ <∼ 1, here ṁ1 is the critical rate of advection-dominated accretion flow (ADAF). In these solutions, the energy loss rate of the ions by Coulomb energy transfer between the ions and electrons is larger than the viscously heating rate and it is the advective heating together with the viscous dissipation that balances the Coulomb cooling of ions. When ṁ1 <∼ ṁ <∼ ṁ2, where ṁ2 ∼ 5ṁ1 < 1, the accretion flow remains hot throughout the disk. When ṁ2 <∼ ṁ <∼ 1, Coulomb interaction will cool the inner region of the disk within a certain radius (rtr ∼ several – tens of Schwarzschild radii or larger depending on the accretion rate and the outer boundary condition) and the disk will collapse onto the equatorial plane and form an optically thick cold annulus. Compared to ADAF, these hot solutions are much more luminous because of the high accretion rate and efficiency, therefore, we name them luminous hot accretion disks.