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On the stability of self-gravitating protoplanetary discs

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Original languageEnglish
Title of host publicationProceedings of the Conference on Towards Other Earths
Subtitle of host publicationDARWIN/TPF and the Search for Extrasolar Terrestrial Planets, 22-25 April 2003
EditorsM. Fridlund, T. Henning
PublisherESA PUBLICATIONS DIVISION C/O ESTEC
Pages555-560
Volume539
ISBN (Print)92-9092-849-2, 2003
StatePublished - 1 Oct 2003

Abstract

It has already been shown, using a local model, that accretion discs with cooling times tcool ≤ 3Ω-1 fragment into gravitationally bound objects, while those with cooling times tcool > 3Ω-1 evolve into a quasi-steady state. We present results of three-dimensional simulations that test if the local result still holds globally. We find that the fragmentation boundary is close to that determined using the local model, but that fragmentation may occur for longer cooling times when the disc is more massive or when the mass is distributed in such a way as to make a particular region of the disc more susceptible to the growth of the gravitational instability. These results have significant implications for the formation of gaseous planets in protoplanetary discs and also for the redistribution of angular momentum which could be driven by the presence of relatively massive, bound objects within the disc.

    Research areas

  • Protoplanetary Discs, Stability

ID: 19679878