Parent volatiles in comet 9P/Tempel 1: Before and after impact

Michael J. Mumma; Michael A. DiSanti; Karen Magee-Sauer; Boncho P. Bonev; Geronimo L. Villanueva; Hideyo Kawakita; Neil Dello Russo; Erika L. Gibb; Geoffrey A. Blake; James E. Lyke; Randall D. Campbell; Joel Aycock; Al Conrad; Grant M. Hill

doi:10.1126/science.1119337

Parent volatiles in comet 9P/Tempel 1: Before and after impact

Michael J. Mumma, Michael A. DiSanti, Karen Magee-Sauer, Boncho P. Bonev, Geronimo L. Villanueva, Hideyo Kawakita, Neil Dello Russo, Erika L. Gibb, Geoffrey A. Blake, James E. Lyke, Randall D. Campbell, Joel Aycock, Al Conrad, Grant M. Hill

Research output: Contribution to journal › Article › peer-review

161 Scopus citations

Abstract

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.

Original language	English (US)
Pages (from-to)	270-274
Number of pages	5
Journal	Science
Volume	310
Issue number	5746
DOIs	https://doi.org/10.1126/science.1119337
State	Published - Oct 14 2005

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@article{5a5603a5b7e64c8a925dff30ae280267,

title = "Parent volatiles in comet 9P/Tempel 1: Before and after impact",

abstract = "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.",

author = "Mumma, {Michael J.} and DiSanti, {Michael A.} and Karen Magee-Sauer and Bonev, {Boncho P.} and Villanueva, {Geronimo L.} and Hideyo Kawakita and {Dello Russo}, Neil and Gibb, {Erika L.} and Blake, {Geoffrey A.} and Lyke, {James E.} and Campbell, {Randall D.} and Joel Aycock and Al Conrad and Hill, {Grant M.}",

year = "2005",

month = oct,

day = "14",

doi = "10.1126/science.1119337",

language = "English (US)",

volume = "310",

pages = "270--274",

journal = "Science",

issn = "0036-8075",

publisher = "American Association for the Advancement of Science",

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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

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VL - 310

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EP - 274

JO - Science

JF - Science

SN - 0036-8075

IS - 5746

ER -

Parent volatiles in comet 9P/Tempel 1: Before and after impact

Abstract

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