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- Michael J. Mumma
- Solar System Exploration Division, NASA Goddard Space Flight Center, Greenbelt, MD 20771, USA.
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- Michael A. DiSanti
- Solar System Exploration Division, NASA Goddard Space Flight Center, Greenbelt, MD 20771, USA.
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- Karen Magee-Sauer
- Solar System Exploration Division, NASA Goddard Space Flight Center, Greenbelt, MD 20771, USA.
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- Boncho P. Bonev
- Solar System Exploration Division, NASA Goddard Space Flight Center, Greenbelt, MD 20771, USA.
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- Geronimo L. Villanueva
- Solar System Exploration Division, NASA Goddard Space Flight Center, Greenbelt, MD 20771, USA.
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- Hideyo Kawakita
- Solar System Exploration Division, NASA Goddard Space Flight Center, Greenbelt, MD 20771, USA.
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- Neil Dello Russo
- Solar System Exploration Division, NASA Goddard Space Flight Center, Greenbelt, MD 20771, USA.
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- Erika L. Gibb
- Solar System Exploration Division, NASA Goddard Space Flight Center, Greenbelt, MD 20771, USA.
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- Geoffrey A. Blake
- Solar System Exploration Division, NASA Goddard Space Flight Center, Greenbelt, MD 20771, USA.
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- James E. Lyke
- Solar System Exploration Division, NASA Goddard Space Flight Center, Greenbelt, MD 20771, USA.
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- Randall D. Campbell
- Solar System Exploration Division, NASA Goddard Space Flight Center, Greenbelt, MD 20771, USA.
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- Joel Aycock
- Solar System Exploration Division, NASA Goddard Space Flight Center, Greenbelt, MD 20771, USA.
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- Al Conrad
- Solar System Exploration Division, NASA Goddard Space Flight Center, Greenbelt, MD 20771, USA.
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- Grant M. Hill
- Solar System Exploration Division, NASA Goddard Space Flight Center, Greenbelt, MD 20771, USA.
書誌事項
- 公開日
- 2005-10-14
- DOI
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- 10.1126/science.1119337
- 公開者
- American Association for the Advancement of Science (AAAS)
この論文をさがす
説明
<jats:p> We quantified eight parent volatiles (H <jats:sub>2</jats:sub> O, C <jats:sub>2</jats:sub> H <jats:sub>6</jats:sub> , HCN, CO, CH <jats:sub>3</jats:sub> OH, H <jats:sub>2</jats:sub> CO, C <jats:sub>2</jats:sub> H <jats:sub>2</jats:sub> , and CH <jats:sub>4</jats:sub> ) 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. </jats:p>
収録刊行物
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- Science
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Science 310 (5746), 270-274, 2005-10-14
American Association for the Advancement of Science (AAAS)
