Computer Science – Numerical Analysis
Scientific paper
Apr 1995
adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1995apj...442..685z&link_type=abstract
Astrophysical Journal (ISSN 0004-637X), vol. 442, no. 2, Part 1, p. 685-693
Computer Science
Numerical Analysis
82
Line Spectra, Protostars, Star Formation, Stellar Mass Accretion, Stellar Models, Stellar Rotation, Numerical Analysis, Radiative Transfer, Spectral Signatures, Velocity Distribution
Scientific paper
We present radiative transfer models of collapsing clouds with rotation and apply them to B335 and IRAS 16293-2422, the two best candidates of protostellar collapse known to date. By including rotation in the manner of Tereby, Shu, & Cassen (1984), we can reproduce the profiles of several molecular lines not only toward the center position, but also toward a grid of positions near the center. We find that the model of B335 by Zhou et al. (1993) is not affected significantly by the presence of rotation. By including rotation, we can reproduce the observations of IRAS 16293-2422 by Menden et al. (1987); hence, we support the infall interpretations of spectral lines from IRAS 16293-2422 proposed by Walker et al. (1986). We also observed the large-scale rotation of IRAS 16293-2422 in the C(18)O J = 2 approaches 1 line. The observed rotation rate is a factor of 6 smaller than that required to explain the small-scale CS data of Menden et al. (1987). This probably means the precollapse cloud has differential rotation, possibly due to more efficient magnetic braking on large scales.
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