Expressions for linearized perturbations in a massive scalar field dominated cosmological model
Sep 18, 199034 pages
Published in:
- Phys.Rev.D 44 (1991) 352-364
Report number:
- CALT-68-1665
Citations per year
Abstract: (APS)
A spatially flat cosmological model dominated by a massive scalar (or pseudoscalar) field (Φ) with the scalar field potential V(Φ)=m2(Φ−Φ(2))2 (where Φ(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.- astrophysics
- field theory: scalar
- field theory: massive
- massive: field theory
- perturbation theory: linear
- energy: density
- model: fluid
- background field
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