The structure of cometary atmospheres. I - Temperature distribution

Details The structure of cometary atmospheres. I - Temperature distribution The structure of cometary atmospheres. I - Temperature distribution

Mar 1976

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1976ap%26ss..40..149s&link_type=abstract

Astrophysics and Space Science, vol. 40, Mar. 1976, p. 149-155.

Astronomy and Astrophysics

Astrophysics

27

Atmospheric Temperature, Comet Heads, Temperature Distribution, Chemical Reactions, Far Infrared Radiation, Infrared Radiation, Solar Radiation

Scientific paper

The temperature distributions in cometary atmospheres at various heliocentric distances for comets of Bennett and Encke types have been calculated by taking into account heating due to the absorption of solar ultraviolet radiation, cooling by H2O far-infrared emission, and various dynamic processes (expansion, advection, and thermal conduction). The agreement of the results with the observations is, in general, satisfactory. The conversion of CH4 and NH3 to CO and N2 through thermochemical reaction with H2O is shown to be impossible since the temperature is too low at a heliocentric distance 1.5 AU, where CO(+) ions begin to be observable.

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