TY - JOUR
T1 - Parent volatiles in comet 9P/Tempel 1
T2 - Before and after impact
AU - Mumma, Michael J.
AU - DiSanti, Michael A.
AU - Magee-Sauer, Karen
AU - Bonev, Boncho P.
AU - Villanueva, Geronimo L.
AU - Kawakita, Hideyo
AU - Dello Russo, Neil
AU - Gibb, Erika L.
AU - Blake, Geoffrey A.
AU - Lyke, James E.
AU - Campbell, Randall D.
AU - Aycock, Joel
AU - Conrad, Al
AU - Hill, Grant M.
PY - 2005/10/14
Y1 - 2005/10/14
N2 - We quantified eight parent volatiles (H2O, C2H 6, HCN, CO, CH3OH, H2CO, C2H 2, and CH4) in the Jupiter-family comet Tempel 1 using high-dispersion infrared spectroscopy in the wavelength range 2.8 to 5.0 micrometers. The abundance ratio for ethane was significantly higher after impact, whereas those for methanol and hydrogen cyanide were unchanged. The abundance ratios in the ejecta are similar to those for most Oort cloud comets, but methanol and acetylene are lower in Tempel 1 by a factor of about 2. These results suggest that the volatile ices in Tempel 1 and in most Oort cloud comets originated in a common region of the protoplanetary disk.
AB - We quantified eight parent volatiles (H2O, C2H 6, HCN, CO, CH3OH, H2CO, C2H 2, and CH4) in the Jupiter-family comet Tempel 1 using high-dispersion infrared spectroscopy in the wavelength range 2.8 to 5.0 micrometers. The abundance ratio for ethane was significantly higher after impact, whereas those for methanol and hydrogen cyanide were unchanged. The abundance ratios in the ejecta are similar to those for most Oort cloud comets, but methanol and acetylene are lower in Tempel 1 by a factor of about 2. These results suggest that the volatile ices in Tempel 1 and in most Oort cloud comets originated in a common region of the protoplanetary disk.
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U2 - 10.1126/science.1119337
DO - 10.1126/science.1119337
M3 - Article
C2 - 16166477
AN - SCOPUS:26844506026
VL - 310
SP - 270
EP - 274
JO - Science
JF - Science
SN - 0036-8075
IS - 5746
ER -