Dark energy from primordial inflationary quantum fluctuations. ArXiv:1006.0368[astro -ph.CO] PRL 105, 121301 (2010) Christophe Ringeval (Louvain University) Teruaki Suyama (Research Center for the Early Universe) Tomo Takahashi (Saga University) Masahide Yamaguchi (Tokyo Institute of Technology) Shuichiro Yokoyama (Nagoya University)
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Dark energy from primordial inflationary quantum fluctuations.
Dark energy from primordial inflationary quantum fluctuations. ArXiv :1006.0368[astro-ph.CO] PRL 105, 121301 (2010). Christophe Ringeval (Louvain University) Teruaki Suyama (Research Center for the Early Universe) Tomo Takahashi (Saga University) - PowerPoint PPT Presentation
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Dark energy from primordial inflationary quantum fluctuations. ArXiv:1006.0368[astro-ph.CO]
PRL 105, 121301 (2010)
Christophe Ringeval (Louvain University)Teruaki Suyama (Research Center for the Early Universe)Tomo Takahashi (Saga University)Masahide Yamaguchi (Tokyo Institute of Technology)Shuichiro Yokoyama (Nagoya University)
The expansion of the universe is accelerating.
From wikipedia
Cosmological constantQuintessence (introduction of a scalar field)Modification of gravity….
Quintessence Acceleration by the potential energy of the scalar field
Freezing type Thawing type
w
tw=-1
w
tw=-1
The scenario
: quintessence field
Quantum diffusion
During primordial inflation, the coarse grained field undergoes random walk.
: quintessence field
Gaussian distribution
During primordial inflation, the coarse grained field undergoes random walk.
The field takes this typical value in our observable universe.
The scenario
We require that this potential energy is responsible for the current accelerated expansion:
The potential energy
Only depends on
(1)
(2)
is completely fixed. (no free parameters)
The scenario
Energy scale of the primordial inflation
If there is a light scalar field such that , and if the primordial inflation has occurred at TeV scale, then the field drives the current accelerated expansion.
The scenario
To summarize,
Some consequences
(1) Reheating temperature
(2) Tensor-to-scalar ratio
(3) Eternal inflation
The number of e-fold required to reach the Bunch-Davies distribution
This can be realized in the eternal inflation.
Observational constraints
Parameters that are varied.
Basic equations
Observations
• Type Ia supernovae (R.Amanullah et al., ApJ. 716, 712 (2010))