Issue |
A&A
Volume 378, Number 3, November II 2001
|
|
---|---|---|
Page(s) | 1024 - 1036 | |
Section | The Sun | |
DOI | https://doi.org/10.1051/0004-6361:20011193 | |
Published online | 15 November 2001 |
Gas-grain chemical models of star-forming molecular clouds as constrained by ISO and SWAS observations
1
Space Science Division, NASA Ames Research Center, MS 245-3, Moffett Field, CA 94035, USA
2
Leiden Observatory, PO Box 9513, 2300 RA Leiden, The Netherlands
Corresponding author: P. Ehrenfreund, pascale@strwchem.strw.leidenuniv.nf
Received:
20
June
2001
Accepted:
27
August
2001
We have investigated the gaseous and solid state molecular composition of
dense interstellar material that periodically experiences processing in the
shock waves associated with ongoing star formation. Our motivation is to
confront these models with the stringent abundance constraints on CO2,
H2O and O2, in both gas and solid phases, that have been set by ISO and
SWAS. We also compare our results with the chemical composition of dark
molecular clouds as determined by ground-based telescopes. Beginning with the
simplest possible model needed to study molecular cloud gas-grain chemistry,
we only include additional processes where they are clearly required to
satisfy one or more of the ISO-SWAS constraints. When CO, N2 and atoms
of N, C and S are efficiently desorbed from grains, a chemical
quasi-steady-state develops after about one million years. We find that
accretion of CO2 and H2O cannot explain the ISO observations; as with previous models, accretion and reaction
of oxygen atoms are necessary although a high O atom abundance can still be
derived from the CO that remains in the gas. The observational constraints on
solid and gaseous molecular oxygen are both met in this model. However, we
find that we cannot explain the lowest abundances seen by SWAS or the
highest atomic carbon abundances found in molecular clouds; additional
chemical processes are required and possible candidates are given. One
prediction of models of this type is that there should be some regions of
molecular clouds which contain high gas phase abundances of H2O, O2 and
NO. A further consequence, we find, is that interstellar grain mantles could
be rich in NH2OH and NO2. The search for these regions, as well as
NH2OH and NO2 in ices and in hot cores, is an important further test of
this scenario. The model can give good agreement with observations of simple
molecules in dark molecular clouds such as TMC-1 and L134N. Despite the fact
that S atoms are assumed to be continously desorbed from grain surfaces, we
find that the sulphur chemistry independently experiences an "accretion
catastrophe" . The S-bearing molecular abundances cease to lie within the
observed range after about
years and this indicates that there
may be at least two efficient surface desorption mechanisms operating in dark
clouds -one quasi-continous and the other operating more sporadically on this
time-scale. We suggest that mantle removal on short time-scales is mediated
by clump dynamics, and by the effects of star formation on longer time-scales.
The applicability of this type of dynamical-chemical model for molecular cloud
evolution is discussed and comparison is made with other models of dark cloud
chemistry.
Key words: molecular data / ISM: abundances / astrochemistry / molecular processes
© ESO, 2001
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