Nonflat power spectrum in inflationary cosmology

Details Nonflat power spectrum in inflationary cosmology Nonflat power spectrum in inflationary cosmology

Feb 1995

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1995phlb..352...14w&link_type=abstract

Physics Letters B, v. 352, p. 14-19

Physics

1

Scientific paper

The nonflat power spectrum in inflationary cosmology based on tensor-scalar gravity is discussed. In the proposed tensor-scalar cosmology, the gravitational scalar field plays the role of the inflation field. After inflation, the universe expands according to a 2/(3) power law; a(t) ~ t2/(3). Under the constraints of the COBE observations, the large scale streaming velocities and sufficient inflation, the spectral index ns of the density perturbation spectrum ranges from 0.98 to 0.65 in the case of h = 0.5 and ΩBh2 = 0.016.

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