Toward inflation models compatible with the no-boundary proposal

Abstract

In this paper, we investigate various inflation models in the context of the no-boundary proposal. We propose that a good inflation model should satisfy three conditions: observational constraints, plausible initial conditions, and naturalness of the model. For various inflation models, we assign the probability to each initial condition using the no-boundary proposal and define a quantitative standard, typicality, to check whether the model satisfies the observational constraints with probable initial conditions. There are three possible ways to satisfy the typicality criterion: there was pre-inflation near the high energy scale, the potential is finely tuned or the inflationary field space is unbounded, or there are sufficient number of fields that contribute to inflation. The no-boundary proposal rejects some of naive inflation models, explains some of traditional doubts on inflation, and possibly, can have observational consequences.

34 pages, 14 figures

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Cited by in corpus (15)

• On the No-Boundary Proposal for Ekpyrotic and Cyclic Cosmologies
• Fuzzy Euclidean wormholes in de Sitter space
• Swampland, Trans-Planckian Censorship and Fine-Tuning Problem for Inflation: Tunnelling Wavefunction to the Rescue
• Fuzzy Euclidean wormholes in anti-de Sitter space
• No-boundary wave function for two-field inflation
• Homogeneous Instantons in Bigravity
• Phantom of the Hartle-Hawking instanton: connecting inflation with dark energy
• Swampland Constraints on No-Boundary Quantum Cosmology
• Why concave rather than convex inflaton potential?
• Suppression of long-wavelength CMB spectrum from the no-boundary initial condition
• Fuzzy Euclidean wormholes in the inflationary universe
• On the geometry of no-boundary instantons in loop quantum cosmology
• Hartle-Hawking wave function and large-scale power suppression of CMB
• Fuzzy instantons in landscape and swampland: review of the Hartle-Hawking wave function and several applications
• Probability of Boundary Conditions in Quantum Cosmology