Dirty silicate models for hot-centered clouds

Details Dirty silicate models for hot-centered clouds Dirty silicate models for hot-centered clouds

Oct 1982

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1982mnras.201..289r&link_type=abstract

Monthly Notices of the Royal Astronomical Society, vol. 201, Oct. 1982, p. 289-302.

Astronomy and Astrophysics

Astronomy

27

B Stars, Cosmic Dust, Infrared Spectra, Molecular Clouds, O Stars, Silicates, Stellar Models, Dirt, Grain Boundaries, Spectral Energy Distribution, Stellar Envelopes, Stellar Evolution, Stellar Mass Ejection, Stellar Temperature

Scientific paper

The suitability of dirty silicate grain models for hot-centered dust clouds is investigated, applying them both to the mean spectrum for hot-centered clouds and to a number of individual clouds. For a class of source whose IR spectra resemble that of the BN object, a double-shell model is required to fit the IR spectra: an outflowing shell of hot dust with an n(r) proportional to r to the -2 density distribution is surrounded by a second shell of cold dust, presumably associated with the ambient cloud of dust and molecules from which the OB star has formed. For the remaining sources modelled, a uniform density distribution gives a good fit to the observed spectra, which suggests that the clouds from which the stars have formed are not in a state of collapse.

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