Astronomy and Astrophysics – Astrophysics
Scientific paper
Sep 1986
adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1986a%26a...166..225g&link_type=abstract
Astronomy and Astrophysics (ISSN 0004-6361), vol. 166, no. 1-2, Sept. 1986, p. 225-236.
Astronomy and Astrophysics
Astrophysics
95
Condensation, Cosmic Dust, Late Stars, M Stars, Stellar Envelopes, Chemical Composition, Dissociation, Ionization Potentials, Iron, Nucleation, Silicon Oxides, Stellar Winds
Scientific paper
The condensation of dust in circumstellar shells around late M-type giants is discussed. it is shown that one has to distinguish between two different situations. The first is that the central star emits only negligible amounts of UV radiation. Then, the chemistry is dominated by neutral radicals. In this case, MgS, Fe and SiO have to be expected as primary condensates. Model calculations for a dust driven wind yields an inner boundary temperature in accord with typical observed values of approximately 1000 K or less. The second situation is that the central star emits sufficient UV radiation causing the elements of low ionization potential to be strongly ionized up to large distances. This should be true for early M-type stars. Then it is argued that the primary condensate is SiO alone which condenses at a substantial lower temperature of approximately 600 K or less which also is in accord with observations.
Gail Hans-Peter
Sedlmayr Erwin
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