Physics
Scientific paper
Mar 1982
adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1982phdt.........4f&link_type=abstract
Ph.D. Thesis Wisconsin Univ., Madison.
Physics
Interstellar Matter, Molecular Clouds, Protostars, Stellar Winds, Supernovae, Electron Energy, Ionization, Shock Waves, Stellar Evolution, Stellar Rotation
Scientific paper
Various aspects of the interaction of stars with their environments are analyzed. In order to begin the investigation of supernova explosions inside interstellar 'bubbles', Sedov's self-similar blast wave structure for a power law density distribution is reviewed. Calculations over the structure are performed to obtain the total energy content, the shock radius evolution, the electron temperature distribution, and the luminosity of such blast waves. The effects of the stellar wind from the most luminous star in the core of the Orion Nebula are reviewed with the aid of far-ultraviolet satellite observations. In Particular, the production of C(+3) and Si(+3) by three processes: X-ray, ultraviolet, and collisiional ionization is analyzed. It is concluded that those ions are likely produced by ultraviolet ionization of the nebular gas. Under the assumption that molecular clouds are turbulent and clumpy, it is shown that rapidly rotating protostars are likely to be formed. The interaction between the rotating protostars and their parent molecular cloud, via a rotationally driven wind, is analyzed. It is then shown that the dissipation of the protostellar rotational energy can maintain the observed dynamical structure and temperatures in the molecular clouds. As a consequence of this interaction it is proposed that the star formation process is self-regulated.
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