The chemical composition and thermal history of the ice of a cometary nucleus

Details The chemical composition and thermal history of the ice of a cometary nucleus The chemical composition and thermal history of the ice of a cometary nucleus

Jun 1983

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1983a%26a...122..171y&link_type=abstract

Astronomy and Astrophysics (ISSN 0004-6361), vol. 122, no. 1-2, June 1983, p. 171-176.

Astronomy and Astrophysics

Astrophysics

39

Chemical Composition, Comet Nuclei, Condensation, Gas Temperature, Ice, Interstellar Gas, Abundance, Data Acquisition, Interstellar Chemistry, Molecular Gases, Vapor Pressure

Scientific paper

The chemical composition of the ice of a cometary nucleus is investigated on the basis of a condensation calculation. Interstellar molecule composition is assumed for the abundance of the gas. Stable molecular species are adopted as the candidate components of the ice. Condensation temperatures of these molecules are calculated as a function of the gas density. It is pointed out that the ice is not a simple condensate of interstellar molecules but their fractionated condensate lacking in very volatile species. It is shown that the major components of the ice are H2O and CO2 with the abundance ratio of (H2O)/(CO2) of about 10. Further-more, the range of the temperature that the ice of a cometary nucleus experienced in the interstellar cloud and in the primordial solar nebula is estimated. It is shown that the upper limit of the temperature is 50 K in the interstellar cloud and 70 K in the primordial solar nebula, and that the ice experienced at least once a temperature higher than around 20 K.

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