  Cold optically thick accretion disks with hot coronae and radial advection
have been investigated. Within the framework of $\alpha$-viscosity models, we
assume that all the mass accretion and angular momentum transport take place in
the cold disk, but that a fraction of the gravitational energy released is
dissipated in the corona. Both the coronal energy dissipation and the advection
heat transport have a stabilization effect on the thermal and viscous
instabilities of the disk. If that more than $\sim 95$ percent of the total
power is dissipated in the corona, then the locally unstable behavior of the
disk is restricted to a relatively narrow spatial region and is found to lie in
a small range of mass accretion rates. The global temporal variability of the
disk can be very mild or may disappear, and which may be applicable to the
low-frequency ($\sim 0.04$~Hz) quasi-periodic oscillations observed in black
hole candidates Cyg X--1 and GRO J0422+32.
