Other
Scientific paper
Feb 2010
adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2010head...11.1806h&link_type=abstract
American Astronomical Society, HEAD meeting #11, #18.06; Bulletin of the American Astronomical Society, Vol. 41, p.687
Other
Scientific paper
The 30 Dor C superbubble in the Large Magellanic Cloud is a large ( 45 pc radius) shell of material swept up by fast stellar winds and supernovae from tens of massive stars in an OB association. Thermal soft X-ray emission is observed, consistent with the predictions of the wind-blown bubble model of Weaver et al (1977). However, that model does not explain the non-thermal X-ray emission observed from this source and a number of other, similar sources. The featureless X-ray spectrum seen from the western rim of 30 Dor C is a well-observed example. Yamaguchi, Bamba and Koyama (2009) interpret this nonthermal emission as synchrotron X-rays from TeV electrons, while Smith and Wang (2004) argue that this explanation is unlikely because the expansion of the bubble is too slow to produce sufficiently energetic particles. We describe some results from our analysis of archival XMM X-ray observations of the western rim of the 30 Dor C superbubble. This work is supported by the contract SV3-73016 between MIT and the Smithsonian Astrophysical Observatory. The Chandra X-Ray Center at the Smithsonian Astrophysical Observatory is operated on behalf of NASA under the contract NAS8-03060.
Allen Glenn E.
Houck John C.
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