Infrared spectroscopy of four carbon stars with 9.8 micron emission from silicate grains

Details Infrared spectroscopy of four carbon stars with 9.8 micron emission from silicate grains Infrared spectroscopy of four carbon stars with 9.8 micron emission from silicate grains

May 1990

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1990aj.....99.1612l&link_type=abstract

Astronomical Journal (ISSN 0004-6256), vol. 99, May 1990, p. 1612-1620. Research supported by the Robert A. Welch Foundation.

Astronomy and Astrophysics

Astronomy

54

Carbon Stars, Emission Spectra, Infrared Spectroscopy, Silicates, Stellar Spectra, M Stars, Spectral Line Width, Stellar Envelopes, Stellar Evolution, Stellar Luminosity

Scientific paper

High-resolution K band and low resolution 4 micron spectra were obtained for four carbon stars showing IR emission by silicate grains. The results of the analysis of the K band spectra show that they are J-type stars. These results, together with published spectral classifications, show that all known carbon stars with a silicate emission feature are J-type stars. The 4 micron spectra are very similar to the spectra of classical J-type carbon stars, and do not show SiO bands that might come from a M giant companion. A binary model with a luminous M giant companion as a source of the silicate grain is rejected. It is proposed that the silicate grains formed from gas ejecta at or before the He-core flash, and that the flash initiates severe mixing, leading to the star's conversion to a J-type carbon star. The ejecta are stored in an accretion disk around a low mass unevolved companion. If it can be shown that the hypothesized accretion disk is stable and may be heated adequately, this binary model appears to account for these peculiar carbon stars.

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