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Global aspects of the formation of γ Cephei b

Published online by Cambridge University Press:  10 November 2011

Siegfried Eggl ,
Markus Gyergyovits  and
Elke Pilat-Lohinger
Siegfried Eggl
Affiliation:
Institute for Astronomy, University of Vienna, 1180 Vienna, Austria email: siegfried.eggl@univie.ac.at
Markus Gyergyovits
Affiliation:
Institute for Astronomy, University of Vienna, 1180 Vienna, Austria email: siegfried.eggl@univie.ac.at
Elke Pilat-Lohinger
Affiliation:
Institute for Astronomy, University of Vienna, 1180 Vienna, Austria email: siegfried.eggl@univie.ac.at
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Abstract

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Discoveries of extrasolar planets in tight binaries are of great scientific value since these systems can be used to gain new insights in planetary development processes. Gamma Cephei, one of the most thoroughly investigated double star systems is hosting a Jovian planet at a distance of about 2 AU from its primary, a 1.4 solar-mass K1 III-IV star (Neuhäuser et al. 2007; Torres 2007). We comprise aspects of dynamical stability, disc heating processes and different giant planet (GP) formation scenarios in order to gain a better understanding of the open questions that remain in explaining the formation of gamma Cephei b.

Keywords

planetary systems: formationbinaries: generalplanetary 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. 411 - 413
Copyright
Copyright © International Astronomical Union 2011

References

Bell, K. R. 1999, ApJ, 526, 411CrossRefGoogle Scholar
Boss, A. P. 2001, ApJ, 563, 367Google Scholar
Dvorak, R., Pilat-Lohinger, E., Funk, B., & Freistetter, F. 2003, A&AL, 398, 1Google Scholar
Haghighipour, N. 2006, ApJ, 644, 543Google Scholar
Hatzes, A. P., Cochran, W. D., Endl, M., McArthur, B., Paulson, D. B., Walker, G. A. H., Campbell, B., & Yang, S. 2003, ApJ, 599, 1383CrossRefGoogle Scholar
Kennedy, G. M. & Kenyon, S. J. 2008, ApJ, 673, 502Google Scholar
Kley, W. & Nelson, R. P. 2008, A&A, 486, 617Google Scholar
Kratter, K. M., Murray-Clay, R. A., & Youdin, A. N. 2010, ApJ, 710, 1375Google Scholar
Lissauer, J. J. 1987, Icarus, 69, 249Google Scholar
Masset, F. 2000, A&AS, 141, 165Google Scholar
Neuhäuser, R., Mugrauer, M., Fukagawa, M., Torres, G., & Schmidt, T. 2007, A&A, 462, 777Google Scholar
Pollack, J. B., Hollenbach, D., Beckwith, S., Simonelli, D. P., Roush, T., & Fong, W. 1994, ApJ, 421, 615Google Scholar
Pollack, J. B., Hubickyj, O., Bodenheimer, P., Lissauer, J. J., Podolak, M., & Greenzweig, Y. 1996, Icarus, 124, 62Google Scholar
Safronov, V. S. 1972, Academy of Sciences USSR, IPSTGoogle Scholar
Thebault, P., Marzari, F., Scholl, H., Turrini, D., & Barbieri, M. 2004, A&A, 427, 1097Google Scholar
Theis, Ch. & Orlova, N. 2004, A&A, 418, 959Google Scholar
Torres, G. 2007, ApJ, 654, 1095CrossRefGoogle Scholar
Xie, J. & Zhou, J. 2009, ApJ, 698, 2066Google Scholar