Other
Scientific paper
Dec 2001
adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2001aas...19915608l&link_type=abstract
American Astronomical Society, 199th AAS Meeting, #156.08; Bulletin of the American Astronomical Society, Vol. 34, p.564
Other
Scientific paper
Disks cannot be too cold, otherwise gravitational instabilities would violently set in. A simple model of self-gravitating accretion disk is presented here and applied to fit and interpret the Spectral Energy Distribution of a sample of Young Stellar Objects. In general, this scenario is likely to be more relevant for younger objects, for which mm observations point to disk masses comparable to that of the central protostar. The key characteristic of the model is the process of self-regulation associated with gravitational instabilities. This is incorporated in our model equations explicitly and significantly modifies the energy budget inside the disk with respect to standard pictures. Dynamical mechanisms related to the physical processes considered by us have been addressed by other authors, especially by means of numerical simulations. The disk self-gravity may thus enhance the long-wavelength emission of protostellar nebulae through the combined effects of increased viscous dissipation (resulting from significant deviations from Keplerian rotation) and of additional heating (responsible for maintaining the disk close to marginal Jeans stability). An investigation of a relatively large sample of YSOs, which includes four T Tauri stars and two FU Orionis objects discussed by us earlier (A&A, 375, 455-468) and a number of Herbig Ae/Be objects, allows us to identify a subsample of objects for which self-gravity may indeed provide an important contribution to the observed infrared excess. The model turns out to be more appealing for FU Orionis objects, while for T Tauri stars the derived values of the physical parameters, such as disk mass and accretion rate, tend to fall outside the generally accepted range.
Bertin Giuseppe
Lodato Giuseppe
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