  In the classic picture of standard thin accretion disks, the viscous heating
is balanced by the radiative cooling through the diffusion process, and the
radiation-pressure-dominated inner disk suffers convective instability.
However, recent simulations have shown that the vertical advection process
owing to the magnetic buoyancy can make significant contribution to the energy
transport. In addition, no convective instability has been found by comparing
the simulation results with the local convective stability criterion. In this
work, following the spirit of simulations, we revisit the vertical structure of
radiation-pressure-dominated thin disks by including the vertical advection
process. Our study indicates a link between the additional energy transport and
the convectively stable property. Thus, the vertical advection not only has
significant contribution to the energy transport, but also plays an important
role to make the disk convectively stable. Our analyses may be helpful to
understand the discrepancy between the classic theory and simulations on
standard thin disks.
