Astronomy and Astrophysics – Astrophysics
Scientific paper
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.
Fukui Yasuo
Nakagawa Naoko
Yamamoto Tadahiro
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