arXiv subjects
Publications and source records attributed to Xingming Chen.
We show that most of hot, optically thin accretion disk models which ignore advective cooling are not self-consistent. We have found new types of optically thin disk solutions where cooling is dominated by radial advection of heat. These new solutions are thermally and viscously stable.
We consider the inner regions of accretion disks surrounding black holes and neutron stars and investigate the nonlinear time dependent evolution of thermal-viscous instabilities. The viscous stress is assumed to be proportional to the gas pressure with the viscosity parameter formulated as $α=\min[α_0 (h/r)^n, α_{\max}]$, where $h$ is the local scale height, $r$ is the distance from the central compact object, and $n$, $α_0$ and $α_{\max}$ are constants. It is found that the disk is unstable for $α$ sufficiently sensitive to $h$ ($n \gapprox 1.2$). The instabilities are globally coherent in the entire unstable region of the disk and, depending on the viscosity parameters, the time variability of the mass accretion rates are manifested as periodic or quasi-periodic oscillations. We show that, the low frequency ($\sim 0.04$~Hz) quasi-periodic oscillations (QPOs) discovered recently in some of the black hole candidates (Cyg~X-1 and GRO~J0422+32) and a low mass X-ray binary (Rapid Burster MXB~1730--335) may be explicable by the thermal-viscous instabilities in accretion disks. The observations of QPOs place constraints on the viscosity parameters and suggest that $(n,α_0)$ $\sim (1.6,30)$ for the Rapid Burster with a $1.4\,\msun$ neutron star. In the case of black hole candidates, the dependence of $α$ on $h/r$ is less steep corresponding to $n \sim 1.2-1.3$ for black holes less than $10\,\msun$.