NASA NTRS · 19790066801
O VI absorption in interstellar cloud surfaces
Abstract
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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Cowie, L. L., Jenkins, E. B., Songaila, A., York, D. G.. 1979-09-01. O VI absorption in interstellar cloud surfaces. https://ntrs.nasa.gov/citations/19790066801
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