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Ice Mantle Formation in the Envelopes of OH/IR Stars

Published online by Cambridge University Press:  07 August 2017

S.B. Charnley  and
R.G. Smith
S.B. Charnley
Affiliation:
Space Science Division, NASA Ames Research Center, California, USA
R.G. Smith
Affiliation:
Dept. of Physics, University of New South Wales, Campbell, Australia

Abstract

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We have computed ice column densities for a sample of O-rich late-type stars.

Water ice is observed in the outflows from several late-type stars (e.g. Smith et al. 1988) and it is of some observational and theoretical importance to understand how common ice mantles may be and how their formation depends upon the physical conditions in the envelope, such as the radial distributions of density and temperature. We have developed a simple theory of the gas-grain interaction in circumstellar shells (Jura & Morris 1985; Charnley et al. 1992) and used it to compute ice column densities (Nice ) and mantle thicknesses (d) for a sample of well-studied OH/IR stars (Herman & Habing 1985). The models are most sensitive to the dust and gas mass loss rates, as well as to the inner radius of the envelope, Ri , which is poorly determined. Representative results are presented in the Table below where Ri was estimated according to the prescription of Herman et al. (1986).

Type
IV. Planetary Nebulae Connection: Evolution from the AGB
Information
Symposium - International Astronomical Union , Volume 155: Planetary Nebulae , 1993 , pp. 329
Copyright
Copyright © Kluwer 1993 

References

Charnley, S.B., Smith, R.G. & Brown, P.D. 1992, in preparation.Google Scholar
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