Relationship between Star and Gas Radial Velocities in the Small Magellanic Cloud

Details Relationship between Star and Gas Radial Velocities in the Small Magellanic Cloud Relationship between Star and Gas Radial Velocities in the Small Magellanic Cloud

Apr 1964

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1964natur.202..377h&link_type=abstract

Nature, Volume 202, Issue 4930, pp. 377-378 (1964).

Physics

12

Scientific paper

As previously reported by Hindman, Kerr and McGee1 and Hindman2, the H-line profiles from the Small Magellanic Cloud are multiple-peaked over a large area of the Cloud. The gas in the various peaks is smoothly distributed in different overlapping regions, and it has been suggested that the gas masses associated with these peaks are separated in space with systematic motions of their own.

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