Warm inflation model building

By M. Bastero-Gil, A. Berera. 2009

172 citations recorded by the source corpus.

We review the main aspects of the warm inflation scenario, focusing on the inflationary dynamics and the predictions related to the primordial spectrum of perturbations, to be compared with the recent cosmological observations. We study in detail three different classes of inflationary models, chaotic, hybrid models and hilltop models, and discuss their embedding into supersymmetric models and the consequences for model building of the warm inflationary dynamics based on first principles calculations. Due to the extra friction term introduced in the inflaton background evolution generated by the dissipative dynamics, inflation can take place generically for smaller values of the field, and larger values of couplings and masses. When the dissipative dynamics dominates over the expansion, in the so-called strong dissipative regime, inflation proceeds with sub-planckian inflaton values. Models can be naturally embedded into a supergravity framework, with sugra corrections suppressed by the Planck mass now under control, for a larger class of K\"ahler potentials. In particular, this provides a simpler solution to the "eta" problem in supersymmetric hybrid inflation, without restricting the K\"ahler potentials compatible with inflation. For chaotic models dissipation leads to a smaller prediction for the tensor-to-scalar ratio and a less tilted spectrum when compared to the cold inflation scenario. We find in particular that a small component of dissipation renders the quartic model now consistent with the current CMB data.

Subfields: Astronomy and Astrophysics, Nuclear and High Energy Physics

View Paper: https://www.semanticscholar.org/paper/acc405f5fe058029189a3b741e49824e183bba9d

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Citations in the corpus

Viscous Cosmology for Early- and Late-Time Universe (2017, result): “During warm inflation T > H (in geometric units), and it turns out that the tensorto-scalar ratio is modified in comparison to the cold inflation case, namely [37]”
Dissipation coefficients from scalar and fermion quantum field interactions (2010, methodology): “In particular, they can be combined with appropriately chosen coupling constants to be applicable in Supersymmetric (SUSY) models, such as often used in cosmological warm inflation model building [9, 18].”
Scale-dependent gravitational waves from a rolling axion (2015, background): “(2)We note that also in warm inflation [29] the tensor-to-scalar ratio is reduced compared to the standard case due to the dissipative effects and the much greater production of scalar with respect to tensor perturbations due to the coupled inflaton [30].”
General dissipation coefficient in low-temperature warm inflation (2012, background): “If the light sector includes, for example, the MSSM fields, we expectm0 ∼ 1 TeV ≪ T for the high temperatures typically involved in warm inflation models [15].”