Molecular envelopes around evolved stars and the origin of planetary nebulae

Details Molecular envelopes around evolved stars and the origin of planetary nebulae Molecular envelopes around evolved stars and the origin of planetary nebulae

Mar 1978

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1978apj...220l..53z&link_type=abstract

Astrophysical Journal, Part 2 - Letters to the Editor, vol. 220, Mar. 1, 1978, p. L53-L56.

Astronomy and Astrophysics

Astronomy

53

Carbon Monoxide, Giant Stars, Late Stars, Planetary Nebulae, Stellar Envelopes, Stellar Evolution, Angular Velocity, Carbon Stars, Infrared Astronomy, Interstellar Gas, M Stars, Microwave Spectra, Silicon Oxides

Scientific paper

A total of 37 late-type giant stars and IRC and CRL infrared sources have been surveyed in the J = 1-0 rotational transition of carbon monoxide. Broad CO emission lines were detected toward six stars. Combination of these results with other CO observations of similar objects suggests that a majority of the red-giant stars with the largest mass-loss rates are carbon-rich (C/O greater than one) or S-type (C/O of the order of one). Infrared surveys tend to support this assertion. It is suggested that these stars will evolve into planetary nebulae of the classical type; i.e., those having a few tenths of a solar mass and radius 0.1-0.7 pc. Most of these should, therefore, show carbon richness in the nebular matter. Planetaries originating from somewhat lower-mass stars (about 1.1 solar masses), such as those found in globular clusters, in the galactic halo, or near the galactic center, have much smaller ionized masses and radii and may be oxygen-rich (O/C greater than one).

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