The Warm Inflation Story

Berera, Arjun

doi:10.3390/universe9060272

Cited by 19 publications

(2 citation statements)

References 240 publications

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“…This quantization scheme reduces to the usual one in the case of cold inflation, as s k → 0 and v k become the standard solutions to the Mukhanov-Sasaki equation. Furthermore, notice that the classical character of thermal fluctuations [38,39] (encapsulated in s k ) is manifest because of the identity operator. In order to compute the variance of χ, recall that s k is a stochastic function, while v k is a deterministic one.…”

Section: Jcap03(2024)003mentioning

confidence: 99%

Monomial warm inflation revisited

Ballesteros,

Pérez Rodríguez,

Pierre

2024

J. Cosmol. Astropart. Phys.

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We revisit the idea that the inflaton may have dissipated part of its energy into a thermal bath during inflation, considering monomial inflationary potentials and three different forms of dissipation rate. Using a numerical Fokker-Planck approach to describe the stochastic dynamics of inflationary fluctuations, we confront this scenario with current bounds on the spectrum of curvature fluctuations and primordial gravitational waves. We also obtain purely analytical approximations that improve over previously used ones in the small dissipation regime for the amplitude of the spectrum and its tilt. We show that only our numerical Fokker-Planck method is accurate, fast and precise enough to test these models against current data. We advocate its use in future studies of warm inflation. We also apply the stochastic inflation formalism to this scenario, finding that the resulting spectrum is the same as the one obtained with standard perturbation theory. We discuss the origin and convenience of using a commonly implemented large thermal correction to the primordial spectrum and the implications of such a term for a specific scenario. Improved bounds on the scalar spectral index will further constrain warm inflation in the near future.

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Section: Jcap03(2024)003mentioning

confidence: 99%

Monomial warm inflation revisited

Ballesteros,

Pérez Rodríguez,

Pierre

2024

J. Cosmol. Astropart. Phys.

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“…For a detailed discussion on how WI is able to satisfy these different conditions, see e.g. ref [27]2.…”

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confidence: 99%

Defying eternal inflation in warm inflation with a negative running

Montefalcone,

Ramos,

Vicente

et al. 2024

J. Cosmol. Astropart. Phys.

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It was pointed out previously [1] that a sufficiently negative running of the spectral index of curvature perturbations from (ordinary i.e. cold) inflation is able to prevent eternal inflation from ever occurring. Here, we reevaluate those original results, but in the context of warm inflation, in which a substantial radiation component (produced by the inflaton) exists throughout the inflationary period. We demonstrate that the same general requirements found in the context of ordinary (cold) inflation also hold true in warm inflation; indeed an even tinier amount of negative running is sufficient to prevent eternal inflation. This is particularly pertinent, as models featuring negative running are more generic in warm inflation scenarios. Finally, the condition for the existence of eternal inflation in cold inflation — that the curvature perturbation amplitude exceed unity on superhorizon scales — becomes more restrictive in the case of warm inflation. The curvature perturbations must be even larger, i.e. even farther out on the potential, away from the part of the potential where observables, e.g. in the Cosmic Microwave Background, are produced.

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The open effective field theory of inflation

Salcedo,

Colas,

Pajer

2024

J. High Energ. Phys.

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In our quest to understand the generation of cosmological perturbations, we face two serious obstacles: we do not have direct information about the environment experienced by primordial perturbations during inflation, and our observables are practically limited to correlators of massless fields, heavier fields and derivatives decaying exponentially in the number of e-foldings. The flexible and general framework of open systems has been developed precisely to face similar challenges. Building on previous work, we develop a Schwinger-Keldysh path integral description for an open effective field theory of inflation, describing the possibly dissipative and non-unitary evolution of the Goldstone boson of time translations interacting with an unspecified environment, under the key assumption of locality in space and time. Working in the decoupling limit, we study the linear and interacting theory in de Sitter and derive predictions for the power spectrum and bispectrum that depend on a finite number of effective couplings organised in a derivative expansion. The smoking gun of interactions with the environment is an enhanced but finite bispectrum close to the folded kinematical limit. We demonstrate the generality of our approach by matching our open effective theory to an explicit model. Our construction provides a standard model to simultaneously study phenomenological predictions as well as quantum information aspects of the inflationary dynamics.

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The Warm Inflation Story

Cited by 19 publications

References 240 publications

Monomial warm inflation revisited

Monomial warm inflation revisited

Defying eternal inflation in warm inflation with a negative running

The open effective field theory of inflation

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