Physics
Scientific paper
May 1991
adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1991phlb..260...21r&link_type=abstract
Physics Letters B, Volume 260, Issue 1-2, p. 21-26.
Physics
8
Scientific paper
We present an approximate estimate, in the slow ``reheating'' scenario, of the late time power spectrum of adiabatic energy density inhomogeneities generated during an early, scalar field dominated, de Sitter inflation epoch, when the scalar field potential, V(Φ) ~ V0 - λΦα (where V0, λ and α are positive parameters). If α is not too large, the power spectrum is fairly sensitive to the value of the Hubble parameter at ``reheating'', except in the α = 4 case (when it only depends logarithmically on the value of this parameter). When α is sufficiently large, the power spectrum is much more sensitive to the value of the Hubble parameter at ``reheating'', than it is to the value of the dimensionless coupling constant (λ multiplied by the appropriate power of V0), which is, therefore, not unduly constrained by observational data; also, in this regime, the slow ``reheating'' prescription resembles the rapid ``reheating'' prescription. For a moderately large α (e.g., α = 8 or 10), the magnitude of the energy density perturbation is consistent with the late time large-scale observational limit, provided the energy scale of inflation is not too high (for α = 8 or 10 it needs to be ~2 × 1010 or 1011 GeV); the dimensionless coupling constant does not have to be small (in both cases it is >~ 10-2).
I am indebted to J. Preskill for valuable advice.
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