Scalar perturbation spectra from warm inflation
By L. M. Hall, I. Moss, A. Berera. 2003
262 citations recorded by the source corpus.
We present a numerical integration of the cosmological scalar perturbation equations in warm inflation. The initial conditions are provided by a discussion of the thermal fluctuations of an inflaton field and thermal radiation using a combination of thermal field theory and thermodynamics. The perturbation equations include the effects of a damping coefficient $\ensuremath{\Gamma}$ and a thermodynamic potential V. We give an analytic expression for the spectral index of scalar fluctuations in terms of a new slow-roll parameter constructed from $\ensuremath{\Gamma}.$ A series of toy models, inspired by spontaneous symmetry breaking and a known form of the damping coefficient, lead to a spectrum with ${n}_{s}g1$ on large scales and ${n}_{s}l1$ on small scales.
Subfields: Astronomy and Astrophysics, Nuclear and High Energy Physics
View Paper: https://www.semanticscholar.org/paper/3fc3b2c7dd030dccb684dc69d2f78c3ec6837d4c
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In Astronomy and Astrophysics
In Nuclear and High Energy Physics
Citations in the corpus
- 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”
- Power spectrum for inflation models with quantum and thermal noises (2013, background): “D 62 (2000) 083517 [arXiv:astro-ph/0006077]; [8] L.”