The Gravitational Radius of an Irradiated Disk
Abstract
We derive an updated, analytic formula for the gravitational radius, r_{g}, of an irradiated, thin disk. For such a disk, the region outside the gravitational radius will produce a thermal wind, while the region interior to the gravitational radius will be stable. We find that r_{g} ~ 1.4 (M_{*}/M_{solar})/(T_{0}/10^{4}K)AU. The value of 1.4AU is approximately one fifth of currently used values. The analysis uses the adiabatic approximation. We argue that the same formula applies for the nonadiabatic, isothermal case.
 Publication:

Publications of the Astronomical Society of Australia
 Pub Date:
 2003
 DOI:
 10.1071/AS03019
 Bibcode:
 2003PASA...20..337L
 Keywords:

 accretion disks;
 hydrodynamics;
 circumstellar matter;
 stars: winds;
 outflows