Some effects of dust formation on O and C stars - Why carbon stars are underabundant

Details Some effects of dust formation on O and C stars - Why carbon stars are underabundant Some effects of dust formation on O and C stars - Why carbon stars are underabundant

Nov 1989

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1989aj.....98.1814l&link_type=abstract

Astronomical Journal (ISSN 0004-6256), vol. 98, Nov. 1989, p. 1814-1819. Research supported by the National Astronomy and Ionosp

Astronomy and Astrophysics

Astronomy

8

Carbon Stars, Cosmic Dust, O Stars, Color-Color Diagram, Infrared Astronomy Satellite, Mira Variables, Photosphere, Stellar Envelopes, Stellar Evolution

Scientific paper

The prominent 'gap' observed in the (25 - 12) micron distribution of IRAS sources, between colors typifying a blackbody photosphere with T of 2000 K or greater and those of a circumstellar shell with T of 1000 K or less, is exhibited only by oxygen-rich stars. Carbon stars do not share this feature. This difference is readily explained by the ability of carbon to form grains at higher temperatures and lower pressures than silicates. Consequently, the evolution of carbon-rich stars, in both the speed of initiating a mass-loss phase and its duration, is more rapid than that of oxygen-rich stars. This explains their apparent underabundance among Miras. Mass loss from red giants begins with the ability to form dust. Oxygen-rich stars have trouble forming dust, but S stars with oxygen concentration roughly equalling the carbon concentration have almost no dust. In the absence of carbon dredge-up, some rare supernova progenitors may be S stars with masses below 9 solar masses. Such objects may provide the 'gentle' supernovae needed to maintain some close binaries intact.

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