A comparative analysis of dissipation coefficients in warm inflation

Abstract

In the warm inflation scenario, the early cosmic acceleration is driven by the inflaton coupled to thermal fields, decaying into radiation and leaving a hot universe populated by relativistic particles after the end of inflation. The interaction is usually modeled by a dissipation coefficient ${\rm Y}$ that contains the microphysics of the model. In this work, we adopt a well-motivated potential $V(\varphi )=\frac{\lambda }{4}{\varphi }^4$ and constrain a variety of ${\rm Y}$ parameterizations by using updated Cosmic Microwave Background data from the \textit{Planck} and \textit{BICEP/Keck Array} collaborations. We also use a Bayesian statistical criterion to compare the observational viability of these models. Our results show a significant improvement in the constraints over past results reported in the literature and also that some of these warm inflation models can be competitive compared to Starobinsky inflation.

14 pages, 3 figures, 1 table; published in JCAP

References in corpus (10)

• BICEP / Keck XIII: Improved Constraints on Primordial Gravitational Waves using Planck, WMAP, and BICEP/Keck Observations through the 2018 Observing Season
• Warm Inflation and its Microphysical Basis
• Warm inflation dissipative effects: predictions and constraints from the Planck data
• Recent developments in warm inflation
• Warm brane inflation with an exponential potential: A consistent realization away from the swampland
• Trans-Planckian censorship and other swampland bothers addressed in warm inflation
• Observational Constraints on Warm Natural Inflation
• Running and running of the running of the scalar spectral index in warm inflation
• A generalized method of constraining Warm Inflation with CMB data
• New limits on warm inflation from pulsar timing arrays

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