Discovery of high-ionization far-ultraviolet line emission from the interstellar medium

Details Discovery of high-ionization far-ultraviolet line emission from the interstellar medium Discovery of high-ionization far-ultraviolet line emission from the interstellar medium

Feb 1990

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1990apj...350..242m&link_type=abstract

Astrophysical Journal, Part 1 (ISSN 0004-637X), vol. 350, Feb. 10, 1990, p. 242-261.

Astronomy and Astrophysics

Astrophysics

84

Emission Spectra, Far Ultraviolet Radiation, Interstellar Matter, Line Spectra, Carbon, Hydrogen Clouds, Oxygen Spectra, Ultraviolet Spectra

Scientific paper

Diffuse, highly ionized line emission from the 1550 lines of C IV and the 1663 lines of O II was discovered on Space Shuttle mission 61-C. The emission-lines ratios are consistent with a single temperature in most directions, although there is some evidence that the emission results from gas with a nonequilibrium ionization balance and a distribution of temperatures. It is concluded that the observation of UV emission is consistent only with a galactic fountain model with a fountain having a mass flux of 6-25 solar mass/yr and a luminosity of (2.5-13) X 10 to the 40th ergs/s.

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