Journal
MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY
Volume 454, Issue 3, Pages 2529-2538Publisher
OXFORD UNIV PRESS
DOI: 10.1093/mnras/stv2128
Keywords
accretion, accretion discs; gravitation; hydrodynamics; instabilities; planets and satellites: formation; protoplanetary discs
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Funding
- German Research Foundation (DFG) [KL 650/8-2, FOR 759]
- ETH Zurich Postdoctoral Fellowship Programme
- Marie Curie Actions for People COFUND program
- DISCSIM project - European Research Council [341137, ERC-2013-ADG]
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We carry out three dimensional radiation hydrodynamical simulations of gravitationally unstable discs to explore the movement of mass in a disc following its initial fragmentation. We find that the radial velocity of the gas in some parts of the disc increases by up to a factor of approximate to 10 after the disc fragments, compared to before. While the movement of mass occurs in both the inward and outward directions, the inwards movement can cause the inner spirals of a self-gravitating disc to become sufficiently dense such that they can potentially fragment. This suggests that the dynamical behaviour of fragmented discs may cause subsequent fragmentation to occur at smaller radii than initially expected, but only after an initial fragment has formed in the outer disc.
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