Phantom of the Hartle-Hawking instanton: connecting inflation with dark energy

Abstract

If the Hartle-Hawking wave function is the correct boundary condition of our universe, the history of our universe will be well approximated by an instanton. Although this instanton should be classicalized at infinity, as long as we are observing a process of each history, we may detect a non-classicalized part of field combinations. When we apply it to a dark energy model, this non-classicalized part of fields can be well embedded to a quintessence and a phantom model, i.e., a quintom model. Because of the property of complexified instantons, the phantomness will be naturally free from a big rip singularity. This phantomness does not cause perturbative instabilities, as it is an effect emergent from the entire wave function. Our work may thus provide a theoretical basis for the quintom models, whose equation of state (EoS) can cross the cosmological constant boundary (CCB) phenomenologically.

20 pages, 7 figures

References in corpus (6)

• Cosmological Evolution of a Quintom Model of Dark Energy
• The Classical Universes of the No-Boundary Quantum State
• The No-Boundary Measure of the Universe
• Theoretical Aspects of Quintom Models
• Toward inflation models compatible with the no-boundary proposal
• Coleman-de Luccia instanton in dRGT massive gravity

Cited by in corpus (6)

• Fuzzy Euclidean wormholes in de Sitter space
• Fuzzy Euclidean wormholes in anti-de Sitter space
• 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
• Two faces of Hawking radiation and thin-shell emission: pair-creation vs. tunneling