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• W1992538026 abstract "A spatially flat cosmological model dominated by a massive scalar (or pseudoscalar) field ($ensuremath{Phi}$) with the scalar field potential $V(ensuremath{Phi})={m}^{2}{(ensuremath{Phi}ensuremath{-}{ensuremath{Phi}}^{(2)})}^{2}$ (where ${ensuremath{Phi}}^{(2)}$ is the value of the scalar field at which the potential vanishes), in the limit in which the length scale corresponding to the scalar field mass $m$ is very much smaller than length scales of cosmological interest (and, in particular, the length scale set by the Hubble parameter), is a tractable approximation of the macrophysics of both the late-time axion-dominated scenario as well as the early-time reheating subscenario of the inflation picture. Extending techniques we have previously developed, we derive solutions of the synchronous-gauge relativistic linear perturbation equations which govern the evolution of spatial irregularities, about a spatially homogeneous and isotropic background, in this model." @default.
• W1992538026 created "2016-06-24" @default.
• W1992538026 creator A5062376442 @default.
• W1992538026 date "1991-07-15" @default.
• W1992538026 modified "2023-10-16" @default.
• W1992538026 title "Expressions for linearized perturbations in a massive-scalar-field-dominated cosmological model" @default.
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• W1992538026 doi "https://doi.org/10.1103/physrevd.44.352" @default.
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