G-Bounce Inflation: Towards Nonsingular Inflation Cosmology with Galileon Field
arXiv:1501.03568 · doi:10.1007/JHEP04(2015)130
Abstract
We study a nonsingular bounce inflation model, which can drive the early universe from a contracting phase, bounce into an ordinary inflationary phase, followed by the reheating process. Besides the bounce that avoided the Big-Bang singularity which appears in the standard cosmological scenario, we make use of the Horndesky theory and design the kinetic and potential forms of the lagrangian, so that neither of the two big problems in bouncing cosmology, namely the ghost and the anisotropy problems, will appear. The cosmological perturbations can be generated either in the contracting phase or in the inflationary phase, where in the latter the power spectrum will be scale-invariant and fit the observational data, while in the former the perturbations will have nontrivial features that will be tested by the large scale structure experiments. We also fit our model to the CMB TT power spectrum.
18 pages, 7 figures
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- Pulsar timing array observations as possible hints for nonsingular cosmology
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- Anomalies in the CMB from a cosmic bounce
- Microphysical manifestations of viscosity and consequences for anisotropies in the very early universe
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- Implication of GW170817 for cosmological bounces
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- Implication of island for inflation and primordial perturbations
- Perturbations in generalized Galileon theories
- Stable cosmological solutions in Horndeski theory
- Stochastic collapse
- -essence non-minimally coupled with Gauss-Bonnet invariant for inflation
- Null energy condition violation and beyond Horndeski physics in light of DESI DR2 data
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- Parity-violating primordial gravitational waves from null energy condition violation
- Warm inflation in Horndeski gravity
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- Do JWST reionization (optical depth) puzzle, cosmological tensions, and CMB anomalies imply Harrison-Zel'dovich spectrum?
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