Energy conditions and scalar field cosmology

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dc.contributor.author Westmoreland, Shawn
dc.date.accessioned 2013-05-14T18:11:05Z
dc.date.available 2013-05-14T18:11:05Z
dc.date.issued 2013-05-14
dc.identifier.uri http://hdl.handle.net/2097/15811
dc.description.abstract In this report, we discuss the four standard energy conditions of General Relativity (null, weak, dominant, and strong) and investigate their cosmological consequences. We note that these energy conditions can be compatible with cosmic acceleration provided that a repulsive cosmological constant exists and the acceleration stays within certain bounds. Scalar fields and dark energy, and their relationships to the energy conditions, are also discussed. Special attention is paid to the 1988 Ratra-Peebles scalar field model, which is notable in that it provides a physical self-consistent framework for the phenomenology of dark energy. Appendix B, which is part of joint-research with Anatoly Pavlov, Khaled Saaidi, and Bharat Ratra, reports on the existence of the Ratra-Peebles scalar field tracker solution in a curvature-dominated universe, and discusses the problem of investigating the evolution of long-wavelength inhomogeneities in this solution while taking into account the gravitational back-reaction (in the linear perturbative approximation). en_US
dc.language.iso en_US en_US
dc.publisher Kansas State University en
dc.subject General Relativity en_US
dc.subject Cosmology en_US
dc.subject Scalar fields en_US
dc.subject Energy conditions en_US
dc.subject Dark energy en_US
dc.subject Cosmological constant en_US
dc.title Energy conditions and scalar field cosmology en_US
dc.type Report en_US
dc.description.degree Master of Science en_US
dc.description.level Masters en_US
dc.description.department Department of Physics en_US
dc.description.advisor Bharat Ratra en_US
dc.subject.umi Astronomy (0606) en_US
dc.subject.umi Astrophysics (0596) en_US
dc.subject.umi Theoretical Physics (0753) en_US
dc.date.published 2013 en_US
dc.date.graduationmonth August en_US


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