Astronomy and Astrophysics – Astrophysics
Scientific paper
2002-11-05
Mon.Not.Roy.Astron.Soc. 339 (2003) 1025
Astronomy and Astrophysics
Astrophysics
6 pages, 7 figures, accepted for publication in MNRAS
Scientific paper
10.1046/j.1365-8711.2003.06253.x
Using a local model Gammie (2001) has shown that accretion discs with cooling times t_cool <= 3/Omega fragment into gravitationally bound objects, while those with cooling times t_cool > 3/Omega evolve into a quasi-steady state. We use three-dimensional smoothed particle hydrodynamic simulations of protoplanetary accretion discs to test if the local results hold globally. We find that for disc masses appropriate for T Tauri discs, the fragmentation boundary still occurs at a cooling time close to t_cool = 3/Omega. For more massive discs, which are likely to be present at an earlier stage of the star formation process, fragmentation occurs for longer cooling times, but still within a factor of two of that predicted using a local model. These results have implications not only for planet formation in protoplanetary discs and star formation in AGN discs, but also for the redistribution of angular momentum which could be driven by the presence of relatively massive objects within the accretion disc.
Armitage Philip J.
Bate Matthew R.
Bonnell Ian A.
Rice W. K. M.
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