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Survival of organic compounds in ejecta from hypervelocity impacts on ice

Published online by Cambridge University Press:  03 April 2009

S.A. Bowden ,
J. Parnell  and
M.J. Burchell
S.A. Bowden
Affiliation:
Department of Geology and Petroleum Geology, University of Aberdeen, Aberdeen, AB24 3UE, UK e-mail: s.a.bowden@abdn.ac.uk
J. Parnell
Affiliation:
Department of Geology and Petroleum Geology, University of Aberdeen, Aberdeen, AB24 3UE, UK e-mail: s.a.bowden@abdn.ac.uk
M.J. Burchell
Affiliation:
School of Physical Sciences, Ingram Building, University of Kent, Canterbury, CT2 7NH, UK e-mail: M.J.Burchell@kent.ac.uk
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Abstract

Hypervelocity impacts (HVIs) where organic-bearing ice constitutes the target material are important in several aspects of planetary and space science: (1) sampling of planetary surfaces using a hypervelocity projectile to impact the surface and eject surface materials for measurement or collection by a spacecraft; (2) the transfer of organic material between planetary bodies; and (3) providing energy for chemical processes involving surface materials. While small organic molecules (~6 carbon atoms), if present in surface materials, will likely be present in HVI-ejecta, uncertainty remains for larger organic molecules. It is the larger molecular weight compounds which could constitute direct evidence of life, and thus their survival within an HVI-ejecta plume is of key importance when evaluating strategies for life detection on icy bodies. It is not currently known what large organic molecules, and in what concentrations, may be present on icy bodies in the Solar System, but it is highly likely some will be more chemically stable during a HVI than others. Accordingly, in this study we examined a range of chemicals (β,β carotene, stearic acid and anthracene) with molecular weights between 178 and 536 daltons, and three different types of chemical structure. The compounds were solvated in a dimethylsulfoxide/water mixture and frozen. The frozen targets were impacted with steel spheres 1 and 1.5 mm in diameter at velocities of about 4.9 km s−1. Ice ejected during the impact was collected and underwent chemical analysis. The most labile compound (β,β carotene) was only detected (in small amounts) in the ejecta (and only that emitted at the lowest angles of ejection), although the other compounds were present in larger quantities and at a range of ejection angles. A concentration gradient was observed within the ejecta as a function of angle of ejection. This was not the same for both stearic acid and anthracene: the greatest concentrations of stearic acid were found at shallow angles of ejection whereas anthracene was most abundant at both intermediate and large angles of ejection, implying an inverted concentration gradient. These observations may indicate that organic compounds are variably altered and destroyed during a HVI with ice and that the ejecta plume does not sample the original materials equally at all angles of ejection. Future work is planned and will evaluate fractional survival for a greater range of compound types, impact materials and velocities.

Keywords

ejectahypervelocityiceorganicsurvival
Type
Research Article
Information
International Journal of Astrobiology , Volume 8 , Special Issue 1: Papers from the Astrobiology Society of Britain Conference 2008 , January 2009 , pp. 19 - 25
Copyright
Copyright © Cambridge University Press 2009

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