Issue |
A&A
Volume 447, Number 2, February IV 2006
|
|
---|---|---|
Page(s) | 553 - 576 | |
Section | Interstellar and circumstellar matter | |
DOI | https://doi.org/10.1051/0004-6361:20041198 | |
Published online | 07 February 2006 |
Composition and quantities of dust produced by AGB-stars and returned to the interstellar medium
Zentrum für Astronomie, Universität Heidelberg, Institut für Theoretische Astrophysik, Albert-Überle Str. 2, 69120 Heidelberg, Germany e-mail: gail@ita.uni-heidelberg.de
Received:
30
April
2004
Accepted:
13
September
2005
The composition of the dust mixture and the amounts of dust returned
into the interstellar medium during the evolution of low and intermediate mass
stars on the AGB is calculated by simple models for dust-forming stellar winds
with M-, S-, and C-star chemistry. These models consider the most abundant dust
species formed in circumstellar dust shells, i.e. olivine- and pyroxene-type
silicate grains and iron grains in the case of M-stars, iron grains in the case
of S-stars, and carbon, SiC, and iron grains in the case of C-stars. The
wind models are combined with calculations of synthetic AGB-evolution to
consistently determine the variation of the dust injection rate into the
interstellar medium from AGB-stars with initial mass and metallicity as the
stars evolve along the AGB and change their chemical surface compositions due to
repeated “dredge-up” episodes. Numerical results are presented for initial
stellar masses from 1 to 7 and for metallicities between
and
, which can then be used to calculate chemical evolution models for
the dust content of galaxies.
Key words: circumstellar matter / dust, extinction / stars: mass-loss / stars: winds, outflows / stars: AGB and post-AGB / evolution
© ESO, 2006
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