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

被引：140

作者：

Mumma, MJ ^{[1
]}

DiSanti, MA

Magee-Sauer, K

Bonev, BP

Villanueva, GL

Kawakita, H

Dello Russo, N

Gibb, EL

Blake, GA

Lyke, JE

Campbell, RD

Aycock, J

Conrad, A

Hill, GM

机构：

[1] NASA, Goddard Space Flight Ctr, Solar Syst Explorat Div, Greenbelt, MD 20771 USA

[2] Rowan Univ, Dept Phys & Astron, Glassboro, NJ 08028 USA

[3] Univ Toledo, Dept Phys & Astron, Ritter Astrophys Res Ctr, Toledo, OH 43606 USA

[4] Kyoto Sangyo Univ, Dept Phys, Kita Ku, Kyoto 6038555, Japan

[5] Johns Hopkins Univ, Appl Phys Lab, Space Dept, Planetary Explorat Grp, Laurel, MD 20723 USA

[6] Univ Missouri, Dept Phys & Astron, St Louis, MO 63121 USA

[7] CALTECH, Div Geol & Planetary Sci, Pasadena, CA 91125 USA

[8] WM Keck Observ, Kamuela, HI 96743 USA

来源：

SCIENCE | 2005年 / 310卷 / 5746期

关键词：

D O I：

10.1126/science.1119337

中图分类号：

O [数理科学和化学]; P [天文学、地球科学]; Q [生物科学]; N [自然科学总论];

学科分类号：

07 ; 0710 ; 09 ;

摘要：

We quantified eight parent votatiles (H(2)O, C(2)H(6), HCN, CO, CH(3)OH, H(2)CO, C(2)H(2), and CH(4)) 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 tower 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.

引用

页码：270 / 274

页数：5

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