X-ray Study of Thermal Composite Supernova Remnants 3C391 and G349.7+0.2

Details X-ray Study of Thermal Composite Supernova Remnants 3C391 and G349.7+0.2 X-ray Study of Thermal Composite Supernova Remnants 3C391 and G349.7+0.2

May 2003

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2003aspc..289..295c&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

Scientific paper

Supernova remnants 3C391 and G349.7+0.2 are both thermal composites, with shell-like radio emission, interior brightened thermal X-rays, and hydroxyl radical masers characterizing a shock interaction with dense clouds. The normal abundances and high X-ray emitting mass of the two SNRs are indicative of ISM-dominance in the hot gas. This inference, the inner X-ray enhancement, and the molecular lines are in agreement with the notion that both the remnants have been evolving in dense cloudy mediums. Both of their morphologies suggest a scenario in which the remnants have broken out of dense regions into an adjacent region of lower density. The variation of the absorption across 3C391 supports this scenario. G349.7+0.2 is found to be one of the most X-ray-luminous shell-type SNRs known in the Galaxy.

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