Cosmological consequences of a rolling homogeneous scalar field

Details Cosmological consequences of a rolling homogeneous scalar field Cosmological consequences of a rolling homogeneous scalar field

Jun 1988

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1988phrvd..37.3406r&link_type=abstract

Physical Review D (Particles and Fields), Volume 37, Issue 12, 15 June 1988, pp.3406-3427

Mathematics

Logic

1868

Origin And Formation Of The Universe, Lagrangian And Hamiltonian Approach

Scientific paper

The cosmological consequences of a pervasive, rolling, self-interacting, homogeneous scalar field are investigated. A number of models in which the energy density of the scalar field red-shifts in a specific manner are studied. In these models the current epoch is chosen to be scalar-field dominated to agree with dynamical estimates of the density parameter, Ωdyn~0.2, and zero spatial curvature. The required scalar-field potential is ``nonlinear'' and decreases in magnitude as the value of the scalar field increases. A special solution of the field equations which is an attractive, time-dependent, fixed point is presented. These models are consistent with the classical tests of gravitation theory. The Eötvös-Dicke measurements strongly constrain the coupling of the scalar field to light (nongravitational) fields. Nucleosynthesis proceeds as in the standard hot big-bang model. In linear perturbation theory the behavior of baryonic perturbations, in the baryon-dominated epoch, do not differ significantly from the canonical scenario, while the presence of a substantial amount of homogeneous scalar-field energy density at low red-shifts inhibits the growth of perturbations in the baryonic fluid. The energy density in the scalar field is not appreciably perturbed by nonrelativistic gravitational fields, either in the radiation-dominated, matter-dominated, or scalar-field-dominated epochs. On the basis of this effect, we argue that these models could reconcile the low dynamical estimates of the mean mass density with the negligibly small spatial curvature preferred by inflation.

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