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Submitted on August 25, 2005
Accepted on September 9, 2005
Parent Volatiles in Comet 9P/Tempel 1: Before and After Impact
Michael J. Mumma 1*, Michael A. DiSanti 1, Karen Magee-Sauer 2, Boncho P. Bonev 3, Geronimo L. Villanueva 1, Hideyo Kawakita 4, Neil Dello Russo 5, Erika L. Gibb 6, Geoffrey A. Blake 7, James E. Lyke 8, Randall D. Campbell 8, Joel Aycock 8, Al Conrad 8, Grant M. Hill 8
1 Solar System Exploration Division, NASA Goddard Space Flight Center, Greenbelt, MD 20771, USA. 2 Dept. of Physics and Astronomy, Rowan University, Glassboro, NJ 08028-1701, USA. 3 Solar System Exploration Division, NASA Goddard Space Flight Center, Greenbelt, MD 20771, USA; Ritter Astrophysical Research Center, Department of Physics and Astronomy, University of Toledo, Toledo, OH 43606, USA. 4 Department of Physics, Kyoto Sangyo University, Motoyama, Kamigamo, Kita-ku, Kyoto 603-8555, Japan. 5 Space Department, Planetary Exploration Group, Applied Physics Laboratory/Johns Hopkins University, 11100 Johns Hopkins Road, Laurel, MD 20723-6099, USA. 6 Dept. of Physics and Astronomy, University of Missouri - Saint Louis, St. Louis, MO 63121-4499, USA. 7 Division of Geological and Planetary Sciences, California Institute of Technology, Pasadena, CA 91125, USA. 8 W. M. Keck Observatory, 65-1120 Mamalahoa Highway, Kameula, HI 96743, USA.
* To whom correspondence should be addressed.
Michael J. Mumma , E-mail: michael.j.mumma{at}nasa.gov
We quantified eight parent volatiles (H2O, C2H6, HCN, CO, CH3OH,H2CO, C2H2, and CH4) in the Jupiter-family comet Tempel-1 usinghigh-dispersion infrared spectroscopy in the wavelength range2.8-5.0 µm. The abundance ratio for ethane was significantlyhigher after impact (UT 4 July) whereas those for methanol andhydrogen cyanide were unchanged. The abundance ratios in theejecta are similar to most Oort-cloud comets, but methanol andacetylene are lower in Tempel-1 by a factor of about two. Theseresults suggest that the volatile ices in Tempel-1 and in mostOort-cloud comets originated in a common region of the protoplanetarydisk.
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