Abstract for NASA Laboratory Astrophysics Workshop

[Reggie Hudson <hudsonrl@eckerd.edu>]

Hello from NASA-Goddard,

   Attached to this e-mail message is an abstract we are submitting for next
month's NASA Laboratory Astrophysics Workshop.  We're not sure which of us will
attend, but someone certainly will be there to present our work, and so we will
register on site.

   Please note that although the abstract is a TeX file, my LaTeX skills are
rather primitive.  If there are other things needed for this abstract, such as
the authors' affiliations, please let me know.

        Reggie Hudson, Professor of Chemistry
        Eckerd College, St. Petersburg, FL  33733
        http://www.eckerd.edu/academics/chemistry/faculty/hudson
        http://www-691.gsfc.nasa.gov/cosmic.ice.lab



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% Sample abstract for submission to NASA LAW 2006.
% See page 181-183 of Leslie Lamport's LaTeX book (second edition)
% for more info.
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\documentclass{article}

\begin{document}

\title{Investigations into the Astrochemistry of H$_2$O$_2$, O$_2$, and O$_3$ in Ion-Irradiated Ices}

\author{Paul Cooper \and Marla Moore \and Reggie Hudson}

\date{6 January 2006}

\maketitle

\begin{abstract}
Features due to solid-phase H$_2$O$_2$, O$_2$, and O$_3$ have been
found in the reflectance spectra of some of the icy satellites of
Jupiter and Saturn (Spencer and Calvin, 2002; Noll \emph{et al}.,
1997; Carlson \emph{et al}., 1999). These molecules can form by
high-energy jovian magnetospheric and cosmic radiations bombarding
the H$_2$O-ice on the surfaces of these worlds. This radiation
breaks chemical bonds in the ice, forming species that can react to
produce new molecules. Gravitational loss of H$_2$ then leaves an
oxygen-richer ice containing H$_2$O$_2$, O$_2$, and O$_3$. The
radiation chemistries of these three molecules are linked since
H$_2$O$_2$ is a proposed precursor for O$_2$ formation, and O$_2$ is
itself a precursor for O$_3$.

In the Cosmic Ice Laboratory at NASA-Goddard we have studied these
processes by using a 0.8 MeV protons to bombard H$_2$O-ices (Moore
and Hudson, 2000) containing H$_2$O$_2$, O$_2$, and O$_3$.  We are
able to measure rates of molecular formation and destruction, and IR
spectra as a function of temperature, sample concentration, and
radiation dose. In this presentation we show some of our most-recent
results on the radiation chemistries of H$_2$O, H$_2$O$_2$, O$_2$,
and O$_3$, such as the formation of the HO$_3$ radical in irradiated
H$_2$O + O$_3$ ices. Since O$_2$ is now known to be an interstellar
molecule (Liseau \emph{et al}., 2006), our results may also apply to
the chemistry of icy interstellar grain mantles.

\textbf{References:}

 Carlson, R.W., Anderson,
M.S., Johnson, R.E., Smythe, W.D., Hendrix, A.R., Barth, C.A.,
Soderblom, L.A., Hansen, G.B., McCord, T.B., Dalton, J.B., Clark,
R.N., Shirley, J.H., Ocampo, A.C., Matson, D.L., 1999,
\emph{Science}, 283, 2062-2064.

Liseau, R., and Odin team members, 2006, \emph{Proc. IAU Symp. 231},
in press.

Moore, M., Hudson R. L., 2000, \emph{Icarus}, 145, 282-288.

Noll, K.S., Johnson, R.E., Lane, A.L., Domingue, D.L., Weaver, H.A.,
1996, \emph{Science}, 273, 341-343.

Noll, K.S., Roush, T.L., Cruikshank, D.P., Johnson, R.E., Pendleton,
Y.J. 1997, \emph{Nature}, 388, 45-47.

Spencer. J. R., Calvin, W. M., Person, M. J., 1995, \emph{J.
Geophys. Res.} 100, 19049-19056.

Spencer. J. R., Calvin, W. M., 2002, \emph{Astrophys. J.} 124,
3400-3403.

\end{abstract}

\end{document}