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A-8 (BT-7M), A-20, T-34 Model 1940, and T-34 Model 1941
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Sulphur-bearing molecules in AGB stars II: Abundances and distributions
of CS and SiS
Abstract: We surveyed 20 AGB stars of different chemical types using the APEX
telescope, and combined this with an IRAM 30 m and APEX survey of CS and SiS
emission towards over 30 S-type stars. For those stars with detections, we
performed radiative transfer modelling to determine abundances and abundance
distributions. We detect CS towards all the surveyed carbon stars, some S-type
stars, and the highest mass-loss rate oxygen-rich stars ($& 5\times 10^{-6}$
Msol yr$^{-1}$). SiS is detected towards the highest mass-loss rate sources of
all chemical types ($& 8\times 10^{-7}$ Msol yr$^{-1}$). We find CS peak
fractional abundances ranging from ~ $ 4\times 10^{-7}$ to ~ $2\times 10^{-5}$
for the carbon stars, from ~ $ 3\times 10^{-8}$ to ~ $1\times 10^{-7}$ for the
oxygen-rich stars and from ~ $ 1\times 10^{-7}$ to ~ $8\times 10^{-6}$ for the
S-type stars. We find SiS peak fractional abundances ranging from ~ $ 9\times
10^{-6}$ to ~ $ 2\times 10^{-5}$ for the carbon stars, from ~ $ 5\times
10^{-7}$ to ~ $ 2\times 10^{-6}$ for the oxygen-rich stars, and from ~ $
2\times 10^{-7}$ to ~ $ 2\times 10^{-6}$ for the S-type stars. We derived
Si$^{32}$S/Si$^{34}$S = 11.4 for AI Vol, the only star for which we had a
reliable isotopologue detection. Overall, we find that wind density plays an
important role in determining the chemical composition of AGB CSEs. It is seen
that for oxygen-rich AGB stars both CS and SiS are detected only in the highest
density circumstellar envelopes and their abundances are generally lower than
for carbon-rich AGB stars by around an order of magnitude. For carbon-rich and
S-type stars SiS was also only detected in the highest density circumstellar
envelopes, while CS was detected consistently in all surveyed carbon stars and
sporadically among the S-type stars.
Solar and Stellar Astrophysics (astro-ph.SR)
[astro-ph.SR]
[astro-ph.SR] for this version)
Submission history
From: Ta&#ssa Danilovich []
[v1] Fri, 13 Jul :14 GMT
(2496kb,D)
Wed, 1 Aug :53 GMT
(2496kb,D)
