A Determination of the HDO/H 2 O Ratio in Comet C/1995 O1 (Hale-Bopp)-Reference-Cited by-同舟云学术

A Determination of the HDO/H 2 O Ratio in Comet C/1995 O1 (Hale-Bopp)

Published:1998-02-06 Issue:5352 Volume:279 Page:842-844
ISSN:0036-8075
Container-title:Science
language:en
Short-container-title:Science

Author:

Meier Roland¹²³,Owen Tobias C.¹²³,Matthews Henry E.¹²³,Jewitt David C.¹²³,Bockelée-Morvan Dominique¹²³,Biver Nicolas¹²³,Crovisier Jacques¹²³,Gautier Daniel¹²³

Affiliation:

1. R. Meier, T. C. Owen, D. C. Jewitt, N. Biver, University of Hawaii, Institute for Astronomy, 2680 Woodlawn Drive, Honolulu, HI 96822, USA.

2. H. E. Matthews, Herzberg Institute for Astrophysics, National Research Council, Victoria, BC V8X 4M6, Canada, and Joint Astronomy Centre, 660 North A'Ohoku Place, Hilo, HI 96720, USA.

3. D. Bockelée-Morvan, J. Crovisier, D. Gautier, Observatoire de Paris-Meudon, 5 Place Jules Janssen, F-92195 Meudon, Cedex, France.

Abstract

Deuterated water (HDO) was detected in comet C/1995 O1 (Hale-Bopp) with the use of the James Clerk Maxwell Telescope on Mauna Kea, Hawaii. The inferred D/H ratio in Hale-Bopp's water is (3.3 ± 0.8) × 10 −4 . This result is consistent with in situ measurements of comet P/Halley and the value found in C/1996 B2 (Hyakutake). This D/H ratio, higher than that in terrestrial water and more than 10 times the value for protosolar H 2 , implies that comets cannot be the only source for the oceans on Earth.

Publisher

American Association for the Advancement of Science (AAAS)

Subject

Multidisciplinary

Reference30 articles.

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2. Line areas are integrated over a velocity interval of ±3 km s −1 . Sky noise is the dominant source for the statistical uncertainties of the lines. The ratio of the system temperature in the image and signal sideband was f = 1.41. Because the system cannot distinguish between the two sidebands it scales all lines according to the calibrated upper sideband which means that the line area of CH 3 OH 11 2 -11 1 A ± in the lower sideband has to be multiplied by f. To obtain main beam corrected and absolutely calibrated line areas the measured antenna temperature has to be divided by the main beam efficiency η = 0.53 ± 0.05 and re-scaled by a factor of 1.53 (see text).

3. At 850 μm the submillimeter common-user bolometer array (SCUBA) of JCMT uses an array of 37 pixels cooled to around 100 mK.

4. Biver N., et al., Bull. Am. Astron. Soc. 29, 1047 (1997).

5. N. Dello Russo et al. ibid. p. 1050.

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