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Coronae of the Magellanic Clouds

Published online by Cambridge University Press:  04 August 2017

Klaas S. de Boer
Klaas S. de Boer*
Affiliation:
Astronomisches Institut Tübingen, D-7400 Tübingen, F.R. Germany

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A hot gaseous corona was postulated by Spitzer (1956) for the Milky Way as a consequence of the detection of cool interstellar clouds (seen in Call absorption) on paths to stars in the Milky Way halo. Halos around extra galactic systems were proposed by Bahcall and Spitzer (1969) as a possible explanation for the wealth of high redshift absorption line systems in the spectra of quasars. The recording with the International Ultraviolet Explorer (Boggess et al 1978) in 1978 of echelle spectra of R136 and HD38282 in the LMC showed strong absorption lines of the high ionization stage ions CIV and SiIV, due to material with velocities clearly pertaining to locations outside the Milky Way disk (Savage and de Boer 1979). Thus the reality of the galactic corona became established (review de Boer 1984). There is confusion with the words corona (gas – massive component) and halo (location – stars) and I (1984) proposed for the large mass from dynamics MASsive DArk Component, MASDAC.

Type
Interstellar Matter
Information
Symposium - International Astronomical Union , Volume 108: Structure and Evolution of the Magellanic Clouds , 1984 , pp. 375 - 382
Copyright
Copyright © Reidel 1984 

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