Hostname: page-component-745bb68f8f-s22k5 Total loading time: 0 Render date: 2025-01-11T05:28:37.049Z Has data issue: false hasContentIssue false
  • English
  • Français

Conditions for outward migration

Published online by Cambridge University Press:  10 November 2011

Bertram Bitsch  and
Willy Kley
Bertram Bitsch
Affiliation:
Computational Physics, University of Tübingen, 72076 Tübingen, Germany email: [email protected], [email protected]
Willy Kley
Affiliation:
Computational Physics, University of Tübingen, 72076 Tübingen, Germany email: [email protected], [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.

The migration of protoplanets in discs not only depends on the thermodynamics of the ambient disc but also on the orbital parameters of the embedded planet. In the fully radiative regime, planets can migrate outward if their orbital parameters fit in a very small range. We simulate planets in fully radiative discs (and isothermal discs - for reference) and determine the influence of the orbital parameters (a, e and i) and the planetary mass on the migration time scale and direction.

Keywords

accretion disksplanetary systems: formationradiative tranferhydrodynamics
Type
Contributed Papers
Information
Proceedings of the International Astronomical Union , Volume 6 , Symposium S276: The Astrophysics of Planetary Systems: Formation, Structure, and Dynamical Evolution , October 2010 , pp. 497 - 498
Copyright
Copyright © International Astronomical Union 2011

References

Kley, W., Bitsch, B., & Klahr, H. 2009, A&A, 506, 971Google Scholar
Bitsch, B. & Kley, W. 2010, A&A, 523, A30Google Scholar
Bitsch, B. & Kley, W. 2011, A&A, 530, A41Google Scholar