Other
Scientific paper
Jan 1995
adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1995phdt.........4y&link_type=abstract
Thesis (PH.D.)--UNIVERSITY OF MINNESOTA, 1995.Source: Dissertation Abstracts International, Volume: 56-07, Section: B, page: 380
Other
Supernova Remnants, Stellar Winds, Star Formation
Scientific paper
In order to search for Supernova Remnants (SNRs) and understand the origin of the turbulent gas in Giant H II Regions (GHR), we have taken radio, optical and X -ray observations of several GHRs (NGC 604, NGC 5471, in NGC 2363, and #1 in NGC 2403). The kinematics of the GHRs are studied using TAURUS imaging Fabry-Perot interferometer and echelle spectroscopy in H alpha lambda 6563, (O III) lambda5007 and (S II) lambdalambda6717, 6731 emission lines. Radio continuum observations of the GHRs are taken to detect the synchrotron radiation from SNRs. Since X-ray emission traces the hot gas SNRs and stellar winds produced by heating the interstellar medium, we also analyze the X-ray of NGC 604 to study its diffuse X-ray emission. The physical properties of SNRs inside of GHRs are found to be different from the isolated SNRs, especially these SNRs inside of the expanding shells because of the gas in extremely low density. In this thesis, we studied the possibilities of finding SNRs using kinematical properties and X-ray emission in several nearby GHRs. Both methods showed very promising results. Very high velocity gas (>=200 km s^{ -1}) is detected to be associated with the known SNRs in NGC 5471 and NGC 604. The X-ray study of NGC 604 in this thesis indicate a stronger activity of SNRs inside of the high velocity expanding shells than radio or optical studies. Different mechanisms which may cause the turbulence in the GHRs are studied. While the Virial theorem may be the best explanation for molecular clouds, it is not the case for the GHRs. Our high resolution study of NGC 604 shows that the gas in the expanding shells caused by the stellar winds and the SNRs contribute most to the integrated velocity width of the GHRs. Gravitational motion may have some contributions, but it is small. Other factors like eddy cascade and champagne flow may also have some minor effects. Since the energy generated by the stellar winds and supernovae is related to the number of massive stars which determine the ionizing flux and ionized nebular mass, a rough relation between L and sigma is expected.
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