Identification of two sources of carbon monoxide in comet Hale–Bopp

Michael A. DiSanti (), Michael J. Mumma, Neil Dello Russo, Karen Magee-Sauer, Robert Novak and Terrence W. Rettig
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Michael A. DiSanti: The Catholic University of America
Michael J. Mumma: Laboratory for Extraterrestrial Physics, NASA Goddard Space Flight Center
Neil Dello Russo: The Catholic University of America
Karen Magee-Sauer: Rowan University
Robert Novak: Iona College
Terrence W. Rettig: University of Notre Dame

Nature, 1999, vol. 399, issue 6737, 662-665

Abstract: Abstract The composition of ices in comets may reflect that of the molecular cloud in which the Sun formed, or it may show evidence of chemical processing in the pre-planetary accretion disk around the proto-Sun. As carbon monoxide (CO) is ubiquitous in molecular clouds1,2, its abundance with respect to water could help to determine the degree to which pre-cometary material was processed, although variations in CO abundance may also be influenced by the distance from the Sun at which comets formed3,4,5. Observations have not hitherto provided an unambiguous measure of CO in the cometary ice (native CO). Evidence for an extended source of CO associated with comet Halley was provided by the Giotto spacecraft6,7,8,9, but alternative interpretations exist10. Here we report observations of comet Hale–Bopp which show that about half of the CO in the comet comes directly from ice stored in the nucleus. The abundance of this CO with respect to water (12 per cent) is smaller than in quiescent regions of molecular clouds, but is consistent with that measured in proto-stellar envelopes11, suggesting that the ices underwent some processing before their inclusion into Hale–Bopp. The remaining CO arises in the coma, probably through thermal destruction of more complex molecules.

Date: 1999
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DOI: 10.1038/21378

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