Star dust, mass loss and the late stages of stellar evolution

Details Star dust, mass loss and the late stages of stellar evolution Star dust, mass loss and the late stages of stellar evolution

Aug 1980

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1980jrasc..74..216k&link_type=abstract

Journal of the Royal Astronomical Society of Canada, vol. 74, Aug. 1980, p. 216-233.

Astronomy and Astrophysics

Astronomy

13

Late Stars, Stellar Envelopes, Stellar Evolution, Stellar Mass Ejection, Stellar Models, Stellar Structure, Chemical Composition, Gas Density, Gas Temperature, Interstellar Matter, M Stars, Metallic Stars, Planetary Nebulae, Radiation Pressure, Stellar Temperature, Stellar Winds

Scientific paper

The role of dust grains in the thermal and dynamical structure of the circumstellar envelopes of late-type stars is discussed. It is suggested that radiation pressure on grains is responsible for the large-scale mass loss observed during the late lifetime of a star, and that planetary nebulae are the direct consequence of such mass loss. Since the conditions necessary for grains to form are dependent on the chemical composition of the star, metallicity can be an important parameter in determining the end point of stellar evolution. The association of dust grains with stellar winds also has a significant effect on the interstellar medium. The observed amount of interstellar grains can be supplied by two processes: the ejection of silicate grains from M stars, and the ejection of carbon-based grains from the ionized winds of planetary nebulae and novae.

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