Convective-Dynamical Instability in Radiation-Supported Accretion Disks

Details Convective-Dynamical Instability in Radiation-Supported Accretion Disks Convective-Dynamical Instability in Radiation-Supported Accretion Disks

2000-03-20

arxiv.org/abs/astro-ph/0003286v1

Astronomy and Astrophysics

Astrophysics

20 pages, AAS LaTeX

Scientific paper

10.1086/309217

We study radiation-hydrodynamical normal modes of radiation-supported accretion disks in the WKB limit. It has long been known that in the large optical depth limit the standard equilibrium is unstable to convection. We study how the growth rate depends on location within the disk, optical depth, disk rotation, and the way in which the local dissipation rate depends on density and pressure. The greatest growth rates are found near the disk surface. Rotation stabilizes vertical wavevectors, so that growing modes tend to have nearly-horizontal wavevectors. Over the likely range of optical depths, the linear growth rate for convective instability has only a weak dependence on disk opacity. Perturbations to the dissipation have little effect on convective mode growth rates, but can cause growth of radiation sound waves.

Affiliated with

Also associated with

No associations

Rating

Convective-Dynamical Instability in Radiation-Supported Accretion Disks does not yet have a rating. At this time, there are no reviews or comments for this scientific paper.

If you have personal experience with Convective-Dynamical Instability in Radiation-Supported Accretion Disks, we encourage you to share that experience with our LandOfFree.com community. Your opinion is very important and Convective-Dynamical Instability in Radiation-Supported Accretion Disks will most certainly appreciate the feedback.

Rate now

Comments { 0 }

Profile ID: LFWR-SCP-O-392288