Coronae of the Magellanic Clouds

Details Coronae of the Magellanic Clouds Coronae of the Magellanic Clouds

Sep 1984

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1984iaus..108..375d&link_type=abstract

IN: Structure and evolution of the Magellanic Clouds; Proceedings of the Symposium, Tuebingen, West Germany, September 5-8, 1983

Physics

8

Absorption Spectra, Interstellar Gas, Magellanic Clouds, Milky Way Galaxy, Ultraviolet Spectra, Coronas, Interstellar Matter, Ionized Gases, Wavelengths

Scientific paper

UV absorption line data on Magellanic Cloud (MC) intestellar gas is similar enough to Milky Way galaxy data to suggest that the Galaxy also has a corona. The MC spectra have included C IV, Ca II, Na I, C II, Mg II and 21-cm H I lines. Some definition is lost in surveys of the MC because of the closeness of some of the internal galaxies, which often have seemed to have their own coronae. However, energy balance equations have failed to confirm the presence of coronae in the MC, which may only be heated by supernovae at a rate higher than present in the Galaxy. It is concluded that observational resolution must be raised to 10 km/sec at wavelengths as short as 1000 A to fully characterize the ion stages in the interstellar medium in the MC.

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