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Angular momentum of two collided rarefied preplanetesimals and formation of binaries

Published online by Cambridge University Press:  06 April 2010

Sergei I. Ipatov
Sergei I. Ipatov*
Affiliation:
Catholic University of America, Washington DC, USA email: siipatov@hotmail.com Space Research Institute, Moscow, Russia
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Abstract

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The mean angular momentum associated with the collision of two celestial objects moving in almost circular heliocentric orbits was studied. The results of these studies were used to develop models of the formation of binaries at the stage of rarefied preplanetesimals. The models can explain a greater fraction of binaries formed at greater distances from the Sun. Sometimes there could be two centers of contraction inside the rotating preplanetesimal formed as the result of a collision between two rarefied preplanetesimals. Such formation of binaries could result in binaries with almost the same masses of components separated by a large distance. Formation of a disk around the primary could result because the angular momentum that was obtained by a rarefied preplanetesimal formed by collision was greater than the critical angular momentum for a solid body. One or several satellites of the primary could be formed from the disk.

Keywords

Minor planetsasteroidsKuiper Beltsolar system: formation
Type
Contributed Papers
Information
Proceedings of the International Astronomical Union , Volume 5 , Symposium S263: Icy Bodies of the Solar System , August 2009 , pp. 37 - 40
Copyright
Copyright © International Astronomical Union 2010

References

Cuzzi, J. N., Hogan, R. C., & Shariff, K. 2008, ApJ, 687, 1432CrossRefGoogle Scholar
Ipatov, S. I. 1981a, Inst. of Applied Mathematics Preprint N 101, Moscow, 28 P, in RussianGoogle Scholar
Ipatov, S. I. 1981b, Inst. of Applied Mathematics Preprint N 102, Moscow, 28 P, in RussianGoogle Scholar
Ipatov, S. I. 2000, Migration of celestial bodies in the Solar System, URSS, Moscow, 320 P, in RussianGoogle Scholar
Ipatov, S. I. 2001, LPS XXXII, Abstract #1165Google Scholar
Ipatov, S. I. 2004, AIP Conf. Proc., 713, 277; also http://planetquest1.jpl.nasa.gov/TPFDarwinConf/proceedings/posters/p045.pdfCrossRefGoogle Scholar
Ipatov, S. I. 2009a, LPS XL, Abstract #1021Google Scholar
Ipatov, S. I. 2009b, MNRAS, submitted, http://arxiv.org/abs/0904.3529Google Scholar
Johansen, A., Oishi, J. S., Mac Low, M.-M., Klahr, H., Henning, T., & Youdin, A. 2007, Nature, 448, 1022CrossRefGoogle Scholar
Lyra, W., Johansen, A., Klahr, H., & Piskunov, N. 2008, A&A, 491, L41Google Scholar
Petit, J.-M. et al. 2008, Science, 322, 432CrossRefGoogle Scholar
Richardson, D. R. & Walsh, K. J. 2006, Annu. Rev. Earth Planet. Sci., 34, 47CrossRefGoogle Scholar
Walsh, K. J., Richardson, D. R., & Michel, P. 2008, Nature, 454, 188CrossRefGoogle Scholar