O VI absorption in interstellar cloud surfaces

Details O VI absorption in interstellar cloud surfaces O VI absorption in interstellar cloud surfaces

Sep 1979

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1979apj...232..467c&link_type=abstract

Astrophysical Journal, Part 1, vol. 232, Sept. 1, 1979, p. 467-472.

Astronomy and Astrophysics

Astrophysics

44

Absorption Spectra, Astronomical Spectroscopy, Interstellar Gas, Oxygen Spectra, Correlation Coefficients, Hydrogen Clouds, Line Spectra, Oao 3, Velocity Distribution

Scientific paper

The velocity profiles of O VI absorption lines of 24 stars, observed in early Copernicus surveys, have been compared with the line profiles of Si III (1206.51 A) and N II (1083.99 A). The velocity structures of the O VI lines appear to be correlated with those of the material in the lower ionization stages. It is argued that the O VI absorption arises in the coronal gas of the conductive interface between hot gas, responsible for extended, soft X-ray emission, and cooler interstellar clouds. The velocity broadening of both sets of lines is attributed to motions of the cloud surfaces induced by pressure fluctuations in the interstellar medium.

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