Computer Science – Numerical Analysis
Scientific paper
Mar 1980
adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1980apj...236..567d&link_type=abstract
Astrophysical Journal, Part 1, vol. 236, Mar. 1, 1980, p. 567-576. Research supported by the Japan Society for the Promotion of
Computer Science
Numerical Analysis
43
Cosmic Dust, Interstellar Chemistry, Interstellar Matter, Nucleation, Stellar Envelopes, Stellar Mass Ejection, Abundance, Mass Flow, Numerical Analysis, Pressure Effects, Radiation Pressure
Scientific paper
The nucleation and growth of dust grains in the stellar envelope are investigated for the case of oxygen-rich stars, where the mass loss occurs as a result of the radiation pressure on the dust grains. The number density of grains, the final grain sizes, and the final amount of metals remaining in gaseous states are calculated based on the grain-nucleation theory proposed by Yamamoto and Hasegawa and Draine and Salpeter. It is shown that, even if calculations are based on the Lothe-Pound nucleation rate equation instead of the classical, homogeneous nucleation rate equation, the proposed theory gives a number density of grains quite similar to that based on the classical rate equation. The approximate solution of the flow, in this paper, brings physical insight to the problem of how the formation of grains couples the flow passing the sonic point. The metals in the outer envelope remain in gaseous state by the amount of 1-10% of the initial content for the mass-loss rate of 10 to the -5th solar masses/yr and by less than 1% for the mass-loss rate less than 3 x 10 to the -6th solar masses/yr.
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