Hα Emission from the Magellanic Stream

Details Hα Emission from the Magellanic Stream Hα Emission from the Magellanic Stream

Sep 1996

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1996aas...188.6509w&link_type=abstract

American Astronomical Society, 188th AAS Meeting, #65.09; Bulletin of the American Astronomical Society, Vol. 28, p.932

Astronomy and Astrophysics

Astronomy

Scientific paper

Faint ha emission of EM 0.5 -- 1.0 cmsixpc has been detected from points at the leading edges of the Magellanic Stream clouds MS II, MS III, and MS IV (Weiner & Williams 1996, AJ 111, 1156). We present further observations which map ha emission around the nucleus of the cloud MS IV. We find emission of EM 0.1 -- 0.5 cmsixpc, generally strongest on the leading edge of the cloud as defined by the H small{I} 21-cm contours; a feature in the IRAS 100mu map also appears to be associated with the leading edge and ha. This provides further evidence that the ha is generated by ram pressure heating, as the clouds move through tenuous hot coronal gas in the Galactic halo. The unstable interface between the coronal and Stream gas will eventually destroy the MS clouds; much material may already have been stripped out of the Magellanic Clouds and shredded. The gaseous galactic corona likely exerts a considerable influence on both the orbit of the Magellanic Clouds and the evolution of the Clouds' ISM.

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