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Rapid clump formation in discs of young stellar objects class O-I

Published online by Cambridge University Press:  05 January 2015

Olga P. Stoyanovskaya  and
Valeriy N. Snytnikov
Olga P. Stoyanovskaya
Affiliation:
Boreskov Institute of Catalysis SB RAS Pr. Academika Lavrentieva, 5, 630090, Novosibirsk, Russia email: [email protected], [email protected] Novosibirsk State University, Str. Pirogova, 2, 630090, Novosibirsk, Russia
Valeriy N. Snytnikov
Affiliation:
Boreskov Institute of Catalysis SB RAS Pr. Academika Lavrentieva, 5, 630090, Novosibirsk, Russia email: [email protected], [email protected] Novosibirsk State University, Str. Pirogova, 2, 630090, Novosibirsk, Russia
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Abstract

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The formation of planetesimals and large bodies in circumstellar discs can be referred to the stage of massive unstable disc emerging due to the gravitational collapse in the molecular cloud. We have simulated the dynamics of gas and boulder clumps in such systems. The features of instability development in massive disc is discussed. Unlike medium-massive discs the massive disc can provide conditions for simultaneous formation of several clumps as a result of overdensity ring fragmentation. We found regimes where 3, 2 or 1 overdensity ring appear in the disc and then fragment into clumps collecting about a half of the disc mass.

Keywords

circumstellar matterYoung Stellar Object (YSO) class O-Igravitational instabilityself-gravitating clump formation
Type
Contributed Papers
Information
Proceedings of the International Astronomical Union , Volume 9 , Issue S310: Complex Planetary Systems , July 2014 , pp. 223 - 224
Copyright
Copyright © International Astronomical Union 2014 

References

Snytnikov, V. N. & Stoyanovskaya, O. P., 2013, MNRAS, 428, 2Google Scholar
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