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http://hdl.handle.net/11375/21352
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DC Field | Value | Language |
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dc.contributor.advisor | Burgess, Cliff | - |
dc.contributor.author | Horbatsch, Michael | - |
dc.date.accessioned | 2017-05-03T19:42:06Z | - |
dc.date.available | 2017-05-03T19:42:06Z | - |
dc.date.issued | 2008-10 | - |
dc.identifier.uri | http://hdl.handle.net/11375/21352 | - |
dc.description.abstract | Stellar structure is investigated within the framework of scalar-tensor gravity. Novel perturbative analytical results are obtained for constant-density stars and for Newtonian polytropes in the quadratic model with coupling function A(Φ) = exp(αΦ+1/2βΦ^2). They are compared to full numerical calculations, and possible applications to main-sequence stars, white dwarfs, and the Chandrasekhar mass are indicated. It is found that Buchdahl's theorem is violated in Brans-Dicke theory for stars with exponentially-decaying density profiles. However, the mass-to-radius ratio M/R tends to the constant-density value in a certain limit. It is observed that for β < 0, there exists a maximum value of η = P0/ρo for constant-density stars, where P0 and ρ0 are the central pressure and density, respectively. It is conjectured that if such a maximum value also exists for other equations of state, and is less than the constant-density maximum value, then knowledge of P/ρ in the centre of a star can be used to constrain β. | en_US |
dc.language.iso | en_US | en_US |
dc.subject | stellar structure, scalar-tensor, gravity, Newtonian polytropes, mass, radius, density | en_US |
dc.title | Stellar Structure in Scalar-Tensor Gravity | en_US |
dc.type | Thesis | en_US |
dc.contributor.department | Physics and Astronomy | en_US |
dc.description.degreetype | Thesis | en_US |
dc.description.degree | Master of Science (MSc) | en_US |
Appears in Collections: | Digitized Open Access Dissertations and Theses |
Files in This Item:
File | Description | Size | Format | |
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Horbatsch_Michael_2008Oct_Masters..pdf | 4.22 MB | Adobe PDF | View/Open |
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