Multiwavelength observations of the Loop I superbubble

Details Multiwavelength observations of the Loop I superbubble Multiwavelength observations of the Loop I superbubble

Dec 1999

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1999phdt.........4n&link_type=abstract

Thesis (PhD). THE PENNSYLVANIA STATE UNIVERSITY, Source DAI-B 60/08, p. 4009, Feb 2000, 165 pages.

Computer Science

3

Scientific paper

Archival ROSAT PSPC data, IRAS Sky Survey Atlas images, 21 cm data obtained with the NRAO 140-foot telescope, and high-resolution optical spectra obtained with the NOAO Coudé feed telescope are used to investigate the geometrical and spectroscopic properties of the Loop I superbubble and its surrounding medium. Twenty-two fields distributed across the northern half of Loop I are selected to study the variation of the spectroscopic properties. X-ray shadows cast by HI clouds are seen in most of the ROSAT ¼ keV band images. The 4 location of the HI clouds and their LSR velocities have been determined based on 21 cm and optical observations of background stars. Many HI clouds have velocities similar to those determined from previous observations of the expanding shells of Loop I and the LHB, and therefore are probably associated with them. A characteristic radius of the Loop I superbubble is estimated to be about 100 pc. The X-ray spectra extracted from PSPC data are best fitted with a four-component model consisting of an unabsorbed foreground (LHB) emission, background power- law emission, and an absorbed two-temperature thermal plasma emission. The X-ray emission from the interior of the Loop I superbubble can be represented by a two- temperature thermal emission whose temperatures vary from field to field. X-ray emission from the Galactic halo and bulge is noticed in some directions. The energetics and dynamics of the Loop I superbubble are discussed based on the hypothesis that Loop I is powered by stellar wind and supernovae in the Sco-Cen OB association. The observed geometrical and kinematical properties of Loop I are found to be consistent with theoretical predictions based on the standard wind-blown bubble theory. However, the precise history of events in the Sco-Cen OB association must be known to reconcile the difference in the estimates of kinematic age and nuclear age of Loop I. The future of the Loop I superbubble is considered and it is concluded that the Loop I superbubble is unlikely to blow out of the warm HI disk.

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