The evolution of protostellar envelopes of masses 3 solar masses and 10 solar masses. II - Radiation transfer and spectral appearance

Details The evolution of protostellar envelopes of masses 3 solar masses and 10 solar masses. II - Radiation transfer and spectral appearance The evolution of protostellar envelopes of masses 3 solar masses and 10 solar masses. II - Radiation transfer and spectral appearance

May 1980

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1980a%26a....85..215y&link_type=abstract

Astronomy and Astrophysics, vol. 85, no. 1-2, May 1980, p. 215-220.

Astronomy and Astrophysics

Astrophysics

51

Protostars, Radiative Transfer, Stellar Envelopes, Stellar Evolution, Cosmic Dust, Equations Of Motion, Hydrodynamic Equations

Scientific paper

The detailed non-grey radiation transfer problem is solved simultaneously with the hydrodynamic equations of motion and continuity for collapsing spherically symmetric prostellar clouds of masses 3Msun and 10Msun. The hydrodynamic results are given in a previous paper (Yorke, 1979a, Paper I). In the present investigation we are chiefly interested in the radial dependence of the temperatures of the various grain components and the spectral as well as the spatial distribution of the radiative flux over the entire disk. In all cases the envelope surrounding the accreting protostar is initially opaque to the stellar photons and the resulting appearance is that of an extended infrared source, the apparent size of which is wavelength-dependent. A double peaked infrared spectrum (in the far and near IR) as reported by Yorke (1977a) for more massive protostellar envelopes is also found. This phenomenon becomes less evident, however, as less massive envelopes are considered. The evolutionary sequence could be continued to the time at which the core became optically visible. In the 10Msun case this resulted in an expanding compact H II region. Implications of the results are discussed and comparisons with observations are made.

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