Shocked Atomic and Molecular Gas in Supernova Remnants

Details Shocked Atomic and Molecular Gas in Supernova Remnants Shocked Atomic and Molecular Gas in Supernova Remnants

May 2003

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2003aspc..289..199k&link_type=abstract

The Proceedings of the IAU 8th Asian-Pacific Regional Meeting, Volume I, held 2-5 July 2002 at National Center of Sciences, Hito

Astronomy and Astrophysics

Astronomy

9

Scientific paper

HI 21 cm line emission from fast-moving atomic gas has been detected toward 27 SNRs. The HI gas was usually thought to be part of an expanding HI shell, as expected for an old supernova remnant in a uniform medium. But recent studies show that a good (> 20--30%) fraction of these remnants are interacting with molecular clouds and that the fast-moving HI gas in some of these remnants is likely to have been part of the molecular cloud at first. I review the results of recent studies on SNRs interacting with molecular clouds and discuss the implications of the scarcity of supernova remnants with expanding HI shells.

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