Gravity Waves and Primordial Black Holes in Scalar Warm Little Inflation. (arXiv:2105.08045v1 [hep-ph])
<a href="http://arxiv.org/find/hep-ph/1/au:+Bastero_Gil_M/0/1/0/all/0/1">Mar Bastero-Gil</a>, <a href="http://arxiv.org/find/hep-ph/1/au:+Diaz_Blanco_M/0/1/0/all/0/1">Marta Subías Díaz-Blanco</a>
In warm inflation, dissipation due to the interactions of the inflaton field
to other light degrees of freedom leads naturally to the enhancement of the
primordial spectrum during the last 10-20 efolds of inflation. We study this
effect in a variant of the Warm Little Inflaton model, where the inflaton
couples to light scalars, with a quartic chaotic potential. These large
fluctuations on re-entry will form light, evaporating Primordial Black Holes,
with masses lighter than $10^6$ g. But at the same time they will act as a
source for the tensors at second order. The enhancement is maximal near the end
of inflation, which result in a spectral density of Gravitational Waves (GW)
peaked at frequencies $f sim O(10^3-10^5)$ Hz today, and with an amplitude
$Omega_{GW} sim 10^{-10}-10^{-8}$. Although the frequency range is outside
the reach of present and planned GW detectors, it might be reached in future
high-frequency gravitational waves detectors, designed to search for
cosmological stochastic GW backgrounds above MHz frequencies.
In warm inflation, dissipation due to the interactions of the inflaton field
to other light degrees of freedom leads naturally to the enhancement of the
primordial spectrum during the last 10-20 efolds of inflation. We study this
effect in a variant of the Warm Little Inflaton model, where the inflaton
couples to light scalars, with a quartic chaotic potential. These large
fluctuations on re-entry will form light, evaporating Primordial Black Holes,
with masses lighter than $10^6$ g. But at the same time they will act as a
source for the tensors at second order. The enhancement is maximal near the end
of inflation, which result in a spectral density of Gravitational Waves (GW)
peaked at frequencies $f sim O(10^3-10^5)$ Hz today, and with an amplitude
$Omega_{GW} sim 10^{-10}-10^{-8}$. Although the frequency range is outside
the reach of present and planned GW detectors, it might be reached in future
high-frequency gravitational waves detectors, designed to search for
cosmological stochastic GW backgrounds above MHz frequencies.
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