Radiative transfer in dust clouds. III - Circumstellar dust shells around late M giants and supergiants.

Details Radiative transfer in dust clouds. III - Circumstellar dust shells around late M giants and supergiants. Radiative transfer in dust clouds. III - Circumstellar dust shells around late M giants and supergiants.

Feb 1983

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1983mnras.202..767r&link_type=abstract

Monthly Notices of the Royal Astronomical Society, vol. 202, Feb. 1983, p. 767-795, 797-811. Research supported by the Science

Astronomy and Astrophysics

Astronomy

134

Carbon Stars, M Stars, Radiative Transfer, Stellar Envelopes, Stellar Models, Stellar Radiation, Supergiant Stars, Cosmic Dust, Infrared Spectra, Late Stars, Molecular Spectra, Silicates, Stellar Color, Stellar Spectra, Stellar Temperature

Scientific paper

Available observations of 85 late mass-loss stars (M-stars) were analyzed in order to characterize the circumstellar dust shells (CDS) around the stars. The relationships among the emitted spectra and the star temperature, the condensation temperature of the shell grains, and the density distribution, optical depth, and dimensions of the shells were investigated. Successful modeling of the shells was performed using a configuration consisting of a stellar radiation source in a spherical gas cavity in a spherically symmetric cloud of dust composed of dirty silicate grains. The radiative transfer equation developed by the authors is applied to a sample of 44 carbon stars in order to describe their CDSs. All the stars chosen displayed significant IR excesses. The CDSs were successfully modeled, in comparison with observations, using an inverse square density distribution. Amorphous carbon-type grains produced better results than did graphite grains. A temperature of the central blackbody source of 2500 K was determined for the C4-C6 stars, and 2000 K for the C7-C9 stars.

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