Open AccessThe effect of cooling on the global stability of self‐gravitating protoplanetary discs
Author(s) -
Rice W. K. M.,
Armitage P. J.,
Bate M. R.,
Bonnell I. A.
Publication year - 2003
Publication title -
monthly notices of the royal astronomical society
Language(s) - English
Resource type - Journals
SCImago Journal Rank - 2.058
H-Index - 383
eISSN - 1365-2966
pISSN - 0035-8711
DOI - 10.1046/j.1365-8711.2003.06253.x
Subject(s) - physics , astrophysics , accretion (finance) , smoothed particle hydrodynamics , planet , angular momentum , magnetorotational instability , t tauri star , astronomy , star formation , accretion disc , stars , magnetohydrodynamics , plasma , classical mechanics , quantum mechanics
Using a local model, Gammie has shown that accretion discs with cooling times t cool ≤ 3Ω −1 fragment into gravitationally bound objects, while those with cooling times t cool > 3Ω −1 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 = 3Ω −1 . 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 2 of that predicted using a local model. These results have implications not only for planet formation in protoplanetary discs and star formation in active galactic nucleus discs, but also for the redistribution of angular momentum which could be driven by the presence of relatively massive objects within the accretion disc.