The embedded young stars in the Taurus-Auriga molecular cloud. I - Models for spectral energy distributions

Details The embedded young stars in the Taurus-Auriga molecular cloud. I - Models for spectral energy distributions The embedded young stars in the Taurus-Auriga molecular cloud. I - Models for spectral energy distributions

Sep 1993

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1993apj...414..676k&link_type=abstract

Astrophysical Journal, Part 1 (ISSN 0004-637X), vol. 414, no. 2, p. 676-694.

Astronomy and Astrophysics

Astrophysics

220

Molecular Clouds, Pre-Main Sequence Stars, Protostars, Spectral Energy Distribution, Stellar Envelopes, Stellar Rotation, Stellar Spectra, Auriga Constellation, Far Infrared Radiation, Radiative Transfer, Star Formation, Stellar Models, Taurus Constellation

Scientific paper

We describe radiative transfer calculations of infalling, dusty envelopes surrounding pre-main-sequence stars and use these models to derive physical properties for a sample of 21 heavily reddened young stars in the Taurus-Auriga molecular cloud. The density distributions needed to match the FIR peaks in the spectral energy distributions of these embedded sources suggest mass infall rates similar to those predicted for simple thermally supported clouds with temperatures about 10 K. Unless the dust opacities are badly in error, our models require substantial departures from spherical symmetry in the envelopes of all sources. These flattened envelopes may be produced by a combination of rotation and cavities excavated by bipolar flows. The rotating infall models of Terebey et al. (1984) models indicate a centrifugal radius of about 70 AU for many objects if rotation is the only important physical effect, and this radius is reasonably consistent with typical estimates for the sizes of circumstellar disks around T Tauri stars.

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