Abstract
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) α t 2 3 . Under the constraints of the COBE observations, the large scale streaming velocities and sufficient inflation, the spectral index n s of the density perturbation spectrum ranges from 0.98 to 0.65 in the case of h = 0.5 and om B h 2 = 0.016.
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