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Multidimensional Simulations of Type Ia Supernovae and Classical Novae

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dc.contributor.advisor Calder, Alan C en_US
dc.contributor.author Krueger, Brendan Kurt en_US
dc.contributor.other Department of Physics en_US
dc.date.accessioned 2013-05-22T17:34:58Z
dc.date.accessioned 2015-04-24T14:46:56Z
dc.date.available 2013-05-22T17:34:58Z
dc.date.available 2015-04-24T14:46:56Z
dc.date.issued 2012-08-01
dc.identifier Krueger_grad.sunysb_0771E_11047 en_US
dc.identifier.uri http://hdl.handle.net/1951/59739 en_US
dc.identifier.uri http://hdl.handle.net/11401/71305 en_US
dc.description 102 pg. en_US
dc.description.abstract Explosive astrophysical phenomena have historically played a significant role in understanding the universe and our place within it. Stellar explosions are important distance indicators, allowing exploration of the structure and evolution of the universe. They also form and disperse heavy elements that are recycled into new astrophysical objects. Stellar explosions are not a uniform group; the progenitors and mechanisms of stellar explosions vary tremendously. I used multidimensional simulations to study two distinct types of explosions that are believed to result from similar progenitor systems: compact white dwarf stars that accrete matter from stellar companions. The two types of explosions I studied are type Ia supernovae and classical novae. Type Ia supernovae are thought to arise from a thermonuclear explosion originating in the core of an accreting white dwarf and leave no remnant. These events are the premier distance indicators in cosmological studies, but questions remain about systematic biases and intrinsic scatter. My investigation centered on the systematic impact of the central density of the progenitor on the brightness of the supernova. Relating the progenitor's central density to its age provided a theoretical explanation of the observed trend that type Ia supernovae from older stars are dimmer. I also demonstrated the importance of a statistical study of such problems, due to the strongly nonlinear evolution during the explosion. Classical novae are important for the study of circumstellar dust formation and are significant contributors of specific isotopes found in our galaxy. They result from a thermonuclear runaway occurring in the accreted envelope on a white dwarf. Only the envelope is consumed, so the white dwarf remains and the event may recur on time scales of 10<super>4</super> to 10<super>5</super> years. My study made use of a new simulation code specialized for low-Mach number flows, such as convection just prior to the explosion. I developed hydrostatic initial models and physics modules necessary for simulations of classical novae. This problem provided unexpected challenges, but preliminary simulations of convection-driven mixing between the accreted envelope and the underlying white dwarf are underway. Future results will explore the effects of convection, particularly the quantity and mechanisms of mixing. My research into stellar explosions provided important insight into their mechanisms and required considerable development work, which improved our models and will allow more realistic simulations in the future. en_US
dc.description.sponsorship This work is sponsored by the Stony Brook University Graduate School in compliance with the requirements for completion of degree. en_US
dc.format Monograph en_US
dc.format.medium Electronic Resource en_US
dc.language.iso en_US en_US
dc.publisher The Graduate School, Stony Brook University: Stony Brook, NY. en_US
dc.subject.lcsh Physics en_US
dc.subject.other classical novae, computational fluid dynamics, type Ia supernovae en_US
dc.title Multidimensional Simulations of Type Ia Supernovae and Classical Novae en_US
dc.type Dissertation en_US
dc.mimetype Application/PDF en_US
dc.contributor.committeemember Walter, Frederick M en_US
dc.contributor.committeemember Zingale, Michael en_US
dc.contributor.committeemember Stephens, Peter en_US
dc.contributor.committeemember Pleier, Marc-Andr?? en_US

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