Hayashi limits for carbon stars and the onset of dust-driven winds

Details Hayashi limits for carbon stars and the onset of dust-driven winds Hayashi limits for carbon stars and the onset of dust-driven winds

Jan 1986

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1986a%26a...154..267l&link_type=abstract

Astronomy and Astrophysics (ISSN 0004-6361), vol. 154, no. 1-2, Jan. 1986, p. 267-273.

Astronomy and Astrophysics

Astrophysics

7

Carbon Stars, Stellar Evolution, Stellar Mass Ejection, Stellar Winds, Abundance, Asymptotic Giant Branch Stars, Electron Density (Concentration), Hertzsprung-Russell Diagram, Opacity

Scientific paper

Hayashi limits are computed for carbon stars on the asymptotic giant branch. With previously published treatments of the opacity of cool, carbon-enriched matter, the derived limit is such that the predicted extreme redward evolution of these stars falls far short of observed effective temperatures as well as of those required for grain condensation in the surface layers. Because these calculations already take account of absorption in the red CN bands, this shortfall implies, contrary to an earlier suggestion, that the enhanced opacity due to these bands is not sufficient to explain the observed evolution of carbon stars to extremely cool temperatures. However, with new opacity calculations - which include the isotopic variants of important diatomic molecules and adopt the observationally-justified microturbulent velocity of 5 km/s - the Hayashi limit shifts to substantially cooler effective temperatures and becomes consistent with the belief that N-type carbon stars subsequently evolve into dust-enshrouded configurations.

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