Evolution of the density parameter in multidimensional cosmology

Details Evolution of the density parameter in multidimensional cosmology Evolution of the density parameter in multidimensional cosmology

Jan 1993

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1993phrvd..47..460s&link_type=abstract

Physical Review D (Particles, Fields, Gravitation, and Cosmology), Volume 47, Issue 2, 15 January 1993, pp.460-467

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Field Theories In Dimensions Other Than Four

Scientific paper

Inflation as a dynamical effect of extra dimensions is discussed from the viewpoint of the evolution of the parameters Ω and q in the physical space. By reducing the dynamics of the models FLRW (k=+/-1)×TD(TD=S1×...×S1) and FLRW (k=0)×SD, where FLRW denotes Friedmann, Lemaître, Robertson, and Walker, to two dimensions it is shown that inflation need not imply Ω~=1 for the present time, i.e., that it does not solve the flatness problem. The energy-momentum tensor of the form Tμν=(ρ,mρ,mρ,mρ,nρ,...,nρ) is assumed. The results are comparable to those obtained by Madsen and Ellis for four-dimensional models N=1, d=11 of supergravity theory.

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