Conductive Evaporation of Spherical Interstellar Gas Clouds

Details Conductive Evaporation of Spherical Interstellar Gas Clouds Conductive Evaporation of Spherical Interstellar Gas Clouds

May 1992

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1992aas...180.2407d&link_type=abstract

American Astronomical Society, 180th AAS Meeting, #24.07; Bulletin of the American Astronomical Society, Vol. 24, p.762

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In this work, we present and analyze a new analytic solution for the saturated (flux-limited) thermal evaporation of a spherical cloud. This work is distinguished from earlier analytic studies by allowing the the thermal conductivity to change continuously from a diffusive to a saturated form, in a manner heretofore employed only in numerical calculations. This closed form solution will be of interest as a computational benchmark. From calculated temperature profiles, we evaluate column densities of carbon, nitrogen, oxygen, neon and silicon ions. In accord with other investigations, we find that ionization equilibrium is far from satisfied, and each ion must be separately tracked. Saturation effects tend to lower predicted column densities, as the thermal interface is narrowed relative to its classical structure.

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