Physics
Scientific paper
Jul 1993
adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1993phdt.........1b&link_type=abstract
Ph.D. Thesis University of Western Ontario, London. Dept. of Astronomy.
Physics
1
Massive Stars, Pre-Main Sequence Stars, Star Formation, Stellar Mass Accretion, Stellar Models, Stellar Physics, Digital Simulation, Giant Stars, Stellar Luminosity, Stellar Temperature, Supermassive Stars
Scientific paper
Pre-main sequence evolutionary tracks have been calculated for a series of massive star models under Hayashi's canonical theory and Stahler's mass accretion paradigm. Canonical pre-main sequence tracks for 15-60 solar mass (SM) stars were calculated with both Cox-Stewart (CS) and Rogers-Iglesias (RI) opacities. The differences between the two sequences were systematically explored. The final pre-main sequence phase of the canonical evolution and the onset of central hydrogen burning is discussed. Arrival of a massive star on the zero age main sequence (ZAMS) is defined and the characteristics of the upper ZAMS models are determined. A systematic investigation of pre-main sequence tracks revealed a boundary in the central density versus central temperature plane, beyond which the models always had a central convective core. In a study of a sequence of accretion models, beyond about 17 SM their characteristics became increasingly more luminous and cooler compared to the same-mass canonical ZAMS models. In the main sequence phase, the accretion build model evolved at essentially the same effective temperature as the canonical model but at a lower luminosity. An upper stellar birthline is proposed, defining a boundary in the Hertzsprung Russell diagram beyond which massive stars first become optically visible.
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