Molecular emission lines from the envelopes of evolved stars

Details Molecular emission lines from the envelopes of evolved stars Molecular emission lines from the envelopes of evolved stars

Feb 1989

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1989a%26a...210...78s&link_type=abstract

Astronomy and Astrophysics (ISSN 0004-6361), vol. 210, no. 1-2, Feb. 1989, p. 78-92.

Astronomy and Astrophysics

Astrophysics

66

Carbon Stars, Emission Spectra, Molecular Spectra, Stellar Envelopes, Stellar Spectra, Abundance, Carbon Isotopes, Carbon Monoxide, Cosmic Dust, Spectral Line Width

Scientific paper

Observations of the CO (J = 1-0), (C-13)O (J = 1-0), HCN (J = 1-0), H(C-13)N (J = 1-0), HC3N (J = 10-9), and NHC (J = 1-0) emission lines from a number of well-known evolved stars are presented. The data are used to derive estimates of mass loss rates, envelope sizes, molecular abundances, and isotope ratios using the molecular excitation model of Morris (1980). A reasonable degree of consistency is found among the population of evolved stars in their envelope composition and isotope ratios. The chemistry in carbon stars appears to be similar to that which occurs in the prototypical object IRC + 10216.

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