Thermally induced mixing of water dominated interstellar ices Article (Published Version) http://sro.sussex.ac.uk Burke, Daren J, Wolff, Angela J, Edridge, John L and Brown, Wendy A (2008) Thermally induced mixing of water dominated interstellar ices. Physical Chemistry Chemical Physics, 10 (32). 4956 - 4967. ISSN 1463-9076 This version is available from Sussex Research Online: http://sro.sussex.ac.uk/id/eprint/48670/ This document is made available in accordance with publisher policies and may differ from the published version or from the version of record. If you wish to cite this item you are advised to consult the publisher’s version. Please see the URL above for details on accessing the published version. Copyright and reuse: Sussex Research Online is a digital repository of the research output of the University. Copyright and all moral rights to the version of the paper presented here belong to the individual author(s) and/or other copyright owners. To the extent reasonable and practicable, the material made available in SRO has been checked for eligibility before being made available. Copies of full text items generally can be reproduced, displayed or performed and given to third parties in any format or medium for personal research or study, educational, or not-for-profit purposes without prior permission or charge, provided that the authors, title and full bibliographic details are credited, a hyperlink and/or URL is given for the original metadata page and the content is not changed in any way.
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Thermally induced mixing of water dominated interstellar ices
Article (Published Version)
http://sro.sussex.ac.uk
Burke, Daren J, Wolff, Angela J, Edridge, John L and Brown, Wendy A (2008) Thermally induced mixing of water dominated interstellar ices. Physical Chemistry Chemical Physics, 10 (32). 4956 - 4967. ISSN 1463-9076
This version is available from Sussex Research Online: http://sro.sussex.ac.uk/id/eprint/48670/
This document is made available in accordance with publisher policies and may differ from the published version or from the version of record. If you wish to cite this item you are advised to consult the publisher’s version. Please see the URL above for details on accessing the published version.
Copyright and reuse: Sussex Research Online is a digital repository of the research output of the University.
Copyright and all moral rights to the version of the paper presented here belong to the individual author(s) and/or other copyright owners. To the extent reasonable and practicable, the material made available in SRO has been checked for eligibility before being made available.
Copies of full text items generally can be reproduced, displayed or performed and given to third parties in any format or medium for personal research or study, educational, or not-for-profit purposes without prior permission or charge, provided that the authors, title and full bibliographic details are credited, a hyperlink and/or URL is given for the original metadata page and the content is not changed in any way.
This paper is published as part of a PCCP Themed Issue on:
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Guest Editor: Martin McCoustra
Editorial
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Thermally induced mixing of water dominated interstellar ices
Daren J. Burke, Angela J. Wolff, John L. Edridge and Wendy A. Brown*
Received 29th April 2008, Accepted 1st July 2008
First published as an Advance Article on the web 23rd July 2008
DOI: 10.1039/b807220e
Despite considerable attention in the literature being given to the desorption behaviour of smaller
volatiles, the thermal properties of complex organics, such as ethanol (C2H5OH), which are
predicted to be formed within interstellar ices, have yet to be characterized. With this in mind,
reflection absorption infrared spectroscopy (RAIRS) and temperature programmed desorption
(TPD) have been used to probe the adsorption and desorption of C2H5OH deposited on top of
water (H2O) films of various thicknesses grown on highly oriented pyrolytic graphite (HOPG) at
98 K. Unlike many other molecules detected within interstellar ices, C2H5OH has a comparable
sublimation temperature to H2O and therefore gives rise to a complicated desorption profile.
RAIRS and TPD show that C2H5OH is incorporated into the underlying ASW film during
heating, due to a morphology change in both the C2H5OH and H2O ices. Desorption peaks
assigned to C2H5OH co-desorption with amorphous, crystalline (CI) and hexagonal H2O-ice
phases, in addition to C2H5OH multilayer desorption are observed in the TPD. When C2H5OH is
deposited beneath ASW films, or is co-deposited as a mixture with H2O, complete co-desorption
is observed, providing further evidence of thermally induced mixing between the ices. C2H5OH is
also shown to modify the desorption of H2O at the ASW-CI phase transition. This behaviour has
not been previously reported for more commonly studied volatiles found within astrophysical ices.
These results are consistent with astronomical observations, which suggest that gas-phase
C2H5OH is localized in hotter regions of the ISM, such as hot cores.
Introduction
Water (H2O) is one of the most abundant molecular species
observed in the interstellar medium (ISM) and is found in the
form of interstellar ices frozen out on the surface of dust
grains.1 It has been well documented that interstellar dust
grains play a pivotal role in the chemical and molecular
evolutionary processes in the ISM.2–4 These H2O ice covered
grains open up reaction pathways to molecules and atoms that
accrete on the grains that are not available in the gas-phase.
The composition of interstellar ices is dominated by H2O,
which comprises up to 60–70% of the ice,5,6 and therefore
plays a significant role in the chemistry of the ISM. Other
major components within these ices include small saturated
molecules such as methanol (CH3OH) and carbon monoxide
(CO). Furthermore, models predict that more complex satu-
rated organics, such as ethanol (C2H5OH), which are formed
via grain surface chemistry, are also present within these
ices.7–10 It has been estimated that the C2H5OH composition
within these ices lies between 0.5% and 5% relative to H2O.9
However, infrared space observatory (ISO) data suggests the
upper limit of solid C2H5OH to be 1.2% within these ices.11
The evaporation of these chemically rich icy mantles from
interstellar dust grains has been shown to play a key role in the
chemistry of star-forming regions in the latter stages of devel-
opment, known as hot molecular cores.12–16 Furthermore, the
adsorption and desorption of astrophysical ices are also im-
portant in the sublimation and out-gassing processes of co-
mets17–21 and in regions where shocks lead to sudden heating
of the grains.22–24 Hence to facilitate accurate modelling of
ISM processes, a detailed characterization of the adsorption
and desorption of astrophysically relevant molecules from
H2O covered surfaces is essential. Despite considerable atten-
tion in the literature given to the thermal desorption of simple
volatiles detected in H2O-rich ices,25–33 the desorption of more
complex saturated molecules, such as C2H5OH, has yet to be
explored. We have therefore used reflection absorption infra-
red spectroscopy (RAIRS) and temperature programmed
desorption (TPD) to investigate the adsorption and desorption
of C2H5OH from various thicknesses of amorphous solid
water (ASW) grown on an underlying highly oriented pyroly-
tic graphite (HOPG) surface at 98 K. The exact composition
of interstellar dust grains is still not accurately known and
depends on the astrophysical environment. However, spectro-
scopic observations indicate that these grains are primarily
composed of carbonaceous and silicate material.34,35 The
carbon component of these grains is known to exist in various
forms including graphite, diamond and amorphous carbon.35
Hence the HOPG substrate used in this study can be con-
sidered a suitable dust grain analogue and has previously been
used to investigate the formation of small molecules on model
dust grain surfaces.36,37
The interaction between H2O ice films and astrophysically
relevant gas-phase molecules, and the subsequent annealing of
these model interstellar ices, has received considerable atten-
tion in the literature.25–33 Such processes are of particular
importance to the ISM with regards to elucidatingDepartment of Chemistry, University College London, 20 GordonStreet, London, UK WC1H 0AJ. E-mail: [email protected]
4956 | Phys. Chem. Chem. Phys., 2008, 10, 4956–4967 This journal is �c the Owner Societies 2008
PAPER www.rsc.org/pccp | Physical Chemistry Chemical Physics
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