Hostname: page-component-cd9895bd7-mkpzs Total loading time: 0 Render date: 2024-12-25T17:05:16.617Z Has data issue: false hasContentIssue false
  • English
  • Français

The Gravitational Radius of an Irradiated Disk

Published online by Cambridge University Press:  05 March 2013

Kurt Liffman
Kurt Liffman*
Affiliation:
School of Mathematical Sciences, Monash University, Clayton Vic 3168, Australia Energy and Thermofluids Engineering, CSIRO/MIT, Highett Vic 3190, [email protected]
Rights & Permissions [Opens in a new window]

Abstract

Core share and HTML view are not available for this content. However, as you have access to this content, a full PDF is available via the ‘Save PDF’ action button.

We derive an updated, analytic formula for the gravitational radius, rg, 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 rg ≈ 1.4 (M*/M⊙)/(T0/104K) AU. The value of 1.4 AU is approximately one fifth of currently used values.

The analysis uses the adiabatic approximation. We argue that the same formula applies for the non-adiabatic, isothermal case.

Keywords

accretion diskshydrodynamicscircumstellar matterstars: winds, outflows
Type
Sixth Torino Workshop
Information
Publications of the Astronomical Society of Australia , Volume 20 , Issue 4 , 2003 , pp. 337 - 339
Copyright
Copyright © Astronomical Society of Australia 2003

References

Begelman, M. C., McKee, C. F., & Shields, G. A. 1983, ApJ 271, 70 CrossRefGoogle Scholar
Hollenbach, D., Johnstone, D., Lizano, S., & Shu, F. 1994, ApJ, 428, 654 CrossRefGoogle Scholar
Woods, D. T., Klein, R. I., Castor, J. I., McKee, C. F., & Bell, J. B. 1996, ApJ, 461, 767 CrossRefGoogle Scholar