Perturbation spectra in the warm inflationary scenario
By Andy Taylor, A. Berera. 2000
153 citations recorded by the source corpus.
We investigate the phenomenology of warm inflation and present generic results about the evolution of the inflaton and radiation fields. The general conditions required for warm inflation to take place are derived and discussed. A comprehensive approach is presented for the generation of thermally induced adiabatic and isocurvature perturbations and the amplitude of their spectra calculated. In addition we derive the ratio of tensor-to-scalar perturbations and find the spectral indices for adiabatic, isocurvature and tensor perturbations formed in the warm inflationary era. These results are presented in a simplified and compact approach that is generally applicable. Our results are illustrated by inflation models with polynomial and exponential potentials. We compare our analytic results against numerical models and find excellent agreement. Finally, presently available data is used to put constraints on warm inflation and we discuss how near--future observations may distinguish the warm inflationary scenario from standard supercooled inflation. The main observable difference is the different scalar-to- tensor ratio, and that the consistency relation between this and the slope of tensor perturbations does not hold for warm inflation.
Subfields: Astronomy and Astrophysics, Nuclear and High Energy Physics
View Paper: https://www.semanticscholar.org/paper/4c26fc49a9476a09e290e2e07d64c901b405ef27
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Citations in the corpus
- Power spectrum for inflation models with quantum and thermal noises (2013, result): “In the limit Q ≫ 1 and T ≫ 1 we obtain that Pδφ ∝ T √ HΥ, which is the result found by Berera and Taylor in [7] and also by Hall, Moss and Berera in [8].”
- General dissipation coefficient in low-temperature warm inflation (2012, background): “On one hand, the spectrum of primordial density fluctuations is seeded by thermal rather than vacuum fluctuations of the inflaton field [4, 7–10], which may lead to interesting observational consequences such as the suppression of the tensor-to-scalar ratio and significant deviations from a gaussian”