228 research outputs found
Chemical modeling of Infrared Dark Clouds: the Role of Surface Chemistry
We simulate the chemistry of infrared dark clouds (IRDCs) with a model in
which the physical conditions are homogeneous and time-independent. The
chemistry is solved as a function of time with three networks: one purely
gas-phase, one that includes accretion and desorption, and one, the complete
gas-grain network, that includes surface chemistry in addition. We compare our
results with observed molecular abundances for two representative IRDCs --
IRDC013.90-1 and IRDC321.73-1 -- using the molecular species NH,
HCN, HNC, HCO, HCN, CH, NH and CS. IRDC013.90-1 is a cold IRDC,
with a temperature below 20 K, while IRDC321.73-1 is somewhat warmer, in the
range 20 - 30 K. We find that the complete gas-grain model fits the data very
well, but that the goodness-of-fit is not sharply peaked at a particular
temperature. Surface processes are important for the explanation of the high
gas-phase abundance of NH in IRDC321.73-1. The general success of the
0-D model in reproducing single-dish observations of our limited sample of 8
species shows that it is probably sufficient for an explanation of this type of
data. To build and justify more complicated models, including spatial
temperature and density structure, contraction, and heating, we require
high-resolution interferometric data.Comment: accepted for publication in Ap
O2 signature in thin and thick O2-H2O ices
Aims. In this paper we investigate the detectability of the molecular oxygen
in icy dust grain mantles towards astronomical objects. Methods. We present a
systematic set of experiments with O2-H2O ice mixtures designed to disentangle
how the molecular ratio affects the O2 signature in the mid- and near-infrared
spectral regions. All the experiments were conducted in a closed-cycle helium
cryostat coupled to a Fourier transform infrared spectrometer. The ice mixtures
comprise varying thicknesses from 8 10 to 3 m. The
absorption spectra of the O2-H2O mixtures are also compared to the one of pure
water. In addition, the possibility to detect the O2 in icy bodies and in the
interstellar medium is discussed. Results. We are able to see the O2 feature at
1551 cm even for the most diluted mixture of H2O : O2 = 9 : 1,
comparable to a ratio of O2/H2O = 10 % which has already been detected in situ
in the coma of the comet 67P/Churyumov-Gerasimenko. We provide an estimate for
the detection of O2 with the future mission of the James Webb Space Telescope
(JWST).Comment: 11 pages, 10 figures, article in press, to appear in A&A 201
A Unified Monte Carlo Treatment of Gas-Grain Chemistry for Large Reaction Networks. I. Testing Validity of Rate Equations in Molecular Clouds
In this study we demonstrate for the first time that the unified Monte Carlo
approach can be applied to model gas-grain chemistry in large reaction
networks. Specifically, we build a time-dependent gas-grain chemical model of
the interstellar medium, involving about 6000 gas-phase and 200 grain surface
reactions. This model is used to test the validity of the standard and modified
rate equation methods in models of dense and translucent molecular clouds and
to specify under which conditions the use of the stochastic approach is
desirable.
We found that at temperatures 25--30 K gas-phase abundances of HO,
NH, CO and many other gas-phase and surface species in the stochastic model
differ from those in the deterministic models by more than an order of
magnitude, at least, when tunneling is accounted for and/or diffusion energies
are 3x lower than the binding energies. In this case, surface reactions,
involving light species, proceed faster than accretion of the same species. In
contrast, in the model without tunneling and with high binding energies, when
the typical timescale of a surface recombination is greater than the timescale
of accretion onto the grain, we obtain almost perfect agreement between results
of Monte Carlo and deterministic calculations in the same temperature range. At
lower temperatures ( K) gaseous and, in particular, surface abundances
of most important molecules are not much affected by stochastic processes.Comment: 33 pages, 9 figures, 1 table. Accepted for publication in Ap
Compact dusty clouds and efficient H formation in diffuse ISM
The formation of compact dusty clouds in diffuse interstellar medium (ISM)
has been recently proposed and studied by Tsytovich et al. (2014). In the
present paper, an effect of the clouds on the rate of HH transition in
the ISM is examined. We discuss the mechanisms leading to the formation of the
clouds and the creation of gaseous clumps around them, analyze the main
processes determining the efficiency of the recombination of atomic hydrogen on
dust grains, and estimate the expected enhancement of the global H
formation due to the presence of the clouds. In conclusion, we argue that the
compact dusty clouds provide optimum conditions for the atomic recombination in
diffuse ISM, and point out some astrophysical implications of the resulting
H formation enhancement.Comment: 5 pages, 2 figures, accepted to The Astrophysical Journa
Rotational spectroscopy of the HCCO and DCCO radicals in the millimeter and submillimeter range
The ketenyl radical, HCCO, has recently been detected in the ISM for the
first time. Further astronomical detections of HCCO will help us understand its
gas-grain chemistry, and subsequently revise the oxygen-bearing chemistry
towards dark clouds. Moreover, its deuterated counterpart, DCCO, has never been
observed in the ISM. HCCO and DCCO still lack a broad spectroscopic
investigation, although they exhibit a significant astrophysical relevance. In
this work we aim to measure the pure rotational spectra of the ground state of
HCCO and DCCO in the millimeter and submillimeter region, considerably
extending the frequency range covered by previous studies. The spectral
acquisition was performed using a frequency-modulation absorption spectrometer
between 170 and 650 GHz. The radicals were produced in a low-density plasma
generated from a select mixture of gaseous precursors. For each isotopologue we
were able to detect and assign more than 100 rotational lines. The new lines
have significantly enhanced the previous data set allowing the determination of
highly precise rotational and centrifugal distortion parameters. In our
analysis we have taken into account the interaction between the ground
electronic state and a low-lying excited state (Renner-Teller pair) which
enables the prediction and assignment of rotational transitions with up
to 4. The present set of spectroscopic parameters provides highly accurate,
millimeter and submillimeter rest-frequencies of HCCO and DCCO for future
astronomical observations. We also show that towards the pre-stellar core
L1544, ketenyl peaks in the region where - peaks,
suggesting that HCCO follows a predominant hydrocarbon chemistry, as already
proposed by recent gas-grain chemical models
First ALMA maps of HCO, an important precursor of complex organic molecules, towards IRAS 16293-2422
The formyl radical HCO has been proposed as the basic precursor of many
complex organic molecules such as methanol (CHOH) or glycolaldehyde
(CHOHCHO). Using ALMA, we have mapped, for the first time at high angular
resolution (1, 140 au), HCO towards the Solar-type
protostellar binary IRAS 162932422, where numerous complex organic molecules
have been previously detected. We also detected several lines of the chemically
related species HCO, CHOH and CHOHCHO. The observations revealed
compact HCO emission arising from the two protostars. The line profiles also
show redshifted absorption produced by foreground material of the circumbinary
envelope that is infalling towards the protostars. Additionally, IRAM 30m
single-dish data revealed a more extended HCO component arising from the common
circumbinary envelope. The comparison between the observed molecular abundances
and our chemical model suggests that whereas the extended HCO from the envelope
can be formed via gas-phase reactions during the cold collapse of the natal
core, the HCO in the hot corinos surrounding the protostars is predominantly
formed by the hydrogenation of CO on the surface of dust grains and subsequent
thermal desorption during the protostellar phase. The derived abundance of HCO
in the dust grains is high enough to produce efficiently more complex species
such as HCO, CHOH, and CHOHCHO by surface chemistry. We found that
the main formation route of CHOHCHO is the reaction between HCO and
CHOH.Comment: Accepted in Monthly Notices of the Royal Astronomical Society; 19
pages, 12 figures, 7 table
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