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dc.contributor.authorBauer, Jacoben
dc.date.accessioned2019-09-23T23:10:58Z
dc.date.available2019-09-23T23:10:58Z
dc.identifier.urihttp://hdl.handle.net/1974/26600
dc.description.abstractIn this thesis, we develop and apply a novel algorithm to understand the evolution of stellar discs in ΛCDM cosmological haloes. Three main scientific areas are addressed: the effects of evolving stellar discs on their host haloes, understanding bar formation in cosmological settings, and the formation of vertical disc structure in response to the host halo. First, we find that the presence of central concentrations of baryons in dark matter haloes enhances adiabatic contraction causes an overall modest reduction in substructure. Additionally, the detailed evolution of stellar discs is important for the inner halo density distribution. However, properties of the halo such as the subhalo mass function are broadly unaffected by the evolution of a realistic stellar disc. Next, we find that stellar bars invariably form in Milky Way-like galaxies. The strength of these bars is less dependent on properties like the dynamical temperature of the disc in a cosmological setting. Instead, the disc thickness plays a leading role in determining the overall bar strength. Our discs undergo notable buckling events, yielding present-day pseudobulge-disc-halo systems. We show that these are qualitatively similar to the observed Milky Way. Finally, we show that a wide variety of vertical structure forms when stellar discs are embedded in cosmological haloes. We further show that through a variety of mechanisms, similar vertical structure is excited. By examining twelve simulations of discs in cosmological haloes, we show that the Sgr dSph need not be as massive as 10^{11} solar masses to be consistent with observed vertical structure in the Milky Way. In fact, the recent buckling of the Milky Way’s bar and its present interaction with the LMC are more likely culprits for some of the observed structure in the Milky Way’s thin disc.en
dc.language.isoengen
dc.relation.ispartofseriesCanadian thesesen
dc.rightsAttribution-NonCommercial-ShareAlike 3.0 United Statesen
dc.rightsQueen's University's Thesis/Dissertation Non-Exclusive License for Deposit to QSpace and Library and Archives Canadaen
dc.rightsProQuest PhD and Master's Theses International Dissemination Agreementen
dc.rightsIntellectual Property Guidelines at Queen's Universityen
dc.rightsCopying and Preserving Your Thesisen
dc.rightsThis publication is made available by the authority of the copyright owner solely for the purpose of private study and research and may not be copied or reproduced except as permitted by the copyright laws without written authority from the copyright owner.en
dc.rights.urihttp://creativecommons.org/licenses/by-nc-sa/3.0/us/
dc.subjectGalactic Astronomyen
dc.subjectGalactic Dynamicsen
dc.subjectTheoretical Cosmologyen
dc.subjectNumerical Methodsen
dc.subjectAstrophysicsen
dc.titleNature or Nurture? Collisionless Evolution of Galactic Disc-Halo Systemsen
dc.typethesisen
dc.description.degreePhDen
dc.contributor.supervisorWidrow, Lawrenceen
dc.contributor.departmentPhysics, Engineering Physics and Astronomyen
dc.degree.grantorQueen's University at Kingstonen


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Attribution-NonCommercial-ShareAlike 3.0 United States
Except where otherwise noted, this item's license is described as Attribution-NonCommercial-ShareAlike 3.0 United States