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The structure of cometary atmospheres

I: Temperature distribution

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Abstract

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 dynamical 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 concluded 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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Authors and Affiliations

  1. Institute of Space and Aeronautical Science, University of Tokyo, Tokyo, Japan

    Mikio Shimizu

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  1. Mikio Shimizu
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Shimizu, M. The structure of cometary atmospheres. Astrophys Space Sci 40, 149–155 (1976). https://doi.org/10.1007/BF00651195

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  • DOI: https://doi.org/10.1007/BF00651195

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