Steady models of radiatively modified conductively driven evaporation from interstellar clouds

Details Steady models of radiatively modified conductively driven evaporation from interstellar clouds Steady models of radiatively modified conductively driven evaporation from interstellar clouds

Oct 1987

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1987mnras.228..915b&link_type=abstract

Monthly Notices of the Royal Astronomical Society (ISSN 0035-8711), vol. 228, Oct. 15, 1987, p. 915-931.

Statistics

Computation

61

Computational Astrophysics, Emission Spectra, Evaporation, High Temperature Gases, Interstellar Matter, Molecular Clouds, Astronomical Models, Background Radiation, Hydrodynamic Equations, Ultraviolet Radiation, X Ray Astronomy

Scientific paper

The nonequilibrium ionization structures and radiative loss rates in, and the dynamical structures of conductive interfaces between spherical interstellar clouds and the hot gas in which they are embedded, were calculated self-consistently. The plasmas were assumed to be unmagnetized and only subsonic evaporation was studied. Mass loss rates and the column densities of several observable ions were calculated for interfaces between clouds having a range of radii and being embedded in media with temperatures of 500,000 and 1,000,000 K. The column densities of O(5+), N(4+), and C(3+) in the interfaces are in general compatible with existing ultraviolet absorption data, but the model linewidths may be larger than those observed. If the extreme ultraviolet background emission originates in conductive interfaces around nearby clouds, the pressure of the local interstellar medium must be about 10 to the -11th erg/cu cm; the high pressure conductive interfaces do not produce the observed far ultraviolet emission lines.

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