Grain formation in the expanding gas flow around cool luminous stars

Details Grain formation in the expanding gas flow around cool luminous stars Grain formation in the expanding gas flow around cool luminous stars

Jan 1984

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1984ap%26ss..98...61k&link_type=abstract

Astrophysics and Space Science (ISSN 0004-640X), vol. 98, no. 1, Jan. 1984, p. 61-79.

Astronomy and Astrophysics

Astrophysics

50

Cosmic Dust, Gas Expansion, Interstellar Matter, Stellar Envelopes, Stellar Mass Ejection, Grain Boundaries, Interstellar Extinction, Magnesium, Silicates

Scientific paper

The authors studied grain formation process and flow structure and around cool luminous mass-loss stars. The nucleation and growth theory of Yamamoto and Hasegawa was extended to the case of expanding gas flow. The following stellar parameters were chosen: stellar mass Mhbar = 1 M_sun;, effective temperature Thbar = 3000K, stellar luminosity Lhbar from 7.5×103 to 2.0×104L_sun;, and mass-loss rate |M| from 1.0×10-6 to 1.0×10-4M_sun; yr-1. Main results of the calculations are; (1) grain condensation temperature Tc ≅ 980 ≡ 1080K; (2) total gas pressure at the condensation point Pt ≅ 6×10-11 ≡ 6×10-9 atm; (3) scale parameter Λc ≅ 103 ≡ 6×104; and (4) final grain size rf = 400 Å ≡ 1 μm.

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