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The embedded young stars in the Taurus-Auriga molecular cloud. I - Models for spectral energy distributionsWe 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.
Document ID
Document Type
Reprint (Version printed in journal)
External Source(s)
Kenyon, Scott J. (Harvard-Smithsonian Center for Astrophysics Cambridge, MA, United States)
Calvet, Nuria (Centro de Investigaciones de Astronomia Merida, Venezuela)
Hartmann, Lee (Harvard-Smithsonian Center for Astrophysics Cambridge, MA, United States)
Date Acquired
August 16, 2013
Publication Date
September 10, 1993
Publication Information
Publication: Astrophysical Journal, Part 1
Volume: 414
Issue: 2
ISSN: 0004-637X
Subject Category
Funding Number(s)
Distribution Limits