Hostname: page-component-cd9895bd7-p9bg8 Total loading time: 0 Render date: 2024-12-23T14:42:01.233Z Has data issue: false hasContentIssue false
  • English
  • Français

Formation of massive gas giants on wide orbits

Published online by Cambridge University Press:  10 November 2011

Eduard I. Vorobyov  and
Shantanu Basu
Eduard I. Vorobyov
Affiliation:
Research Institute of Physics, Southern Federal University, Rostov-on-Don, 344090, Russia The Institute for Computational Astrophysics, Saint Mary's University, Halifax, Canada email: [email protected] Dept. of Physics and Astronomy, The University of Western Ontario, London, Canada email: [email protected]
Shantanu Basu
Affiliation:
Dept. of Physics and Astronomy, The University of Western Ontario, London, Canada email: [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 present a mechanism for the formation of massive gas giants on wide orbits via disk fragmentation in the embedded phase of star formation. In this phase, protostellar disks undergo radial pulsations which lead to periodic disk compressions and formation of massive fragments on radial distances of the order of 50–300 AU. The fragments that form during the last episode of disk compression near the end of the embedded phase, when torque from spiral arms become weaker, may survive and mature into massive gas giants. This phenomenon can explain the existence of massive exoplanets on wide orbits is such systems as Fomalhaut and HR 8799.

Keywords

instabilitiesplanetary systems: formationplanetary systems: protoplanetary disks
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. 463 - 464
Copyright
Copyright © International Astronomical Union 2011

References

Dodson-Robinson, S. E., Veras, D., Ford, E. B., & Beichman, C. A. 2010, ApJ, 707, 79Google Scholar
Durisen, R. H., Boss, A. P., Mayer, L., Nelson, A. F., Quinn, T., & Rice, W. K. M. 2007, in Protostars and Planets V, eds. Reipurth, B., Jewitt, D., & Keil, K., University of Arizona Press, Tucson, 607Google Scholar
Kalas, P., Graham, J. R., Chiang, E., Fitzgerald, M. P., Clampin, M., Kite, E. S., Stapelfeldt, K., Marois, C., & Krist, J. 2008, Science, 322, 1345Google Scholar
Lafreniére, D., Jayawardhana, R., & van Kerkwijk, M. H. 2010, ApJ, 719, 497Google Scholar
Marois, C., Macintosh, B., Barman, T., Zuckerman, B., Song, I., Patience, J., Lafreniére, D., & Doyon, R. 2008, Science, 322, 1348Google Scholar
Vorobyov, E. I. & Basu, S. 2006, ApJ, 650, 956Google Scholar
Vorobyov, E. I. & Basu, S. 2010, ApJL, 714, 133CrossRefGoogle Scholar