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Effects of dissipating gas drag on planetesimal accretion in binary systems

Published online by Cambridge University Press:  01 October 2007

Ji-Wei Xie  and
Ji-Lin Zhou
Ji-Wei Xie
Affiliation:
Department of Astronomy, Nanjing University, China email: [email protected]; [email protected]
Ji-Lin Zhou
Affiliation:
Department of Astronomy, Nanjing University, China email: [email protected]; [email protected]
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Abstract

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We numerically investigate the conditions for planetesimal accretion in the circumprimary disk under the perturbing presence of a companion star, with focus on the γ Cephei system. Gas drag is included with a dissipating time scale of 105 years. We show at the beginning(within 103 ∼ 104 years), gas drag damps the ΔV between planetesimals of same sizes and increases ΔV between planetesimals of different sizes. However, after increasing to high values(300∼800m/s), we find the ΔV between bodies of different sizes decrease to very low values (below 10m/s) in a few 105yrs (depending on the gas-dissipating time scale Tdamp, radial size Rp and semi-major axis ap of planetesimals). Hence, the high ΔV is somewhat short-lived, and runaway accretion can be turned on later. We conclude that the conditions for planetary formation in binary systems (even close binary systems) are much better than what we expected before.

Keywords

planetary formationaccretionplanetesimalsbinary stars
Type
Contributed Papers
Information
Proceedings of the International Astronomical Union , Volume 3 , Symposium S249: Exoplanets: Detection, Formation and Dynamics , October 2007 , pp. 419 - 424
Copyright
Copyright © International Astronomical Union 2008

References

Desidera, S. & Barbieri, M. 2007, A&A, 462, 345Google Scholar
Eggenberger, A., Udry, S., & Mayor, M. 2004, A&A, 417, 353Google Scholar
Gladman, B., 1993, Icarus, 106, 247CrossRefGoogle Scholar
Hatzes, A.P., Cochran, W. D., Endl, M., McArthur, B., Paulson, D., Walker, G. A. H., Campbell, B., Yang, S., 2003, ApJ, 599, 1383CrossRefGoogle Scholar
Hayashi, C., 1981, PthPS, 70, 35Google Scholar
Kokubo, E., Yoshinaga, K., & Makino, J. 1998, MNRAS, 297, 1067CrossRefGoogle Scholar
Marzari, F. & Scholl, H. 2000, ApJ, 543, 328CrossRefGoogle Scholar
Thebault, P., Marzari, F., Scholl, H., Turrini, D., Barbieri, M., 2004, A&A, 427, 1097Google Scholar
Thebault, P., Marzari, F., Scholl, H., 2006, Icarus, 183, 193CrossRefGoogle Scholar
Tsukamoto, Y. & Makino, J. 2007, Formation of protoplanets from massive planetesimals in binary systems, eprint arXiv: astro-ph/07072928CrossRefGoogle Scholar
Weidenschilling, S. J. & Davis, D. R., 1985, Icarus, 62, 16CrossRefGoogle Scholar