.png){kind=icon}
Return
What does inflation really predict?
.png){kind=icon}
OA
AI
DOI：10.1088/1475-7516/2005/04/001.png)
.png){kind=icon}
Original request for help.png){kind=icon}
Share.png){kind=icon}
Save
Abstract
En 中文
If the inflaton potential has multiple minima, as may be expected in, e. g., the string theory 'landscape', inflation predicts a probability distribution for the cosmological parameters describing spatial curvature (Omega(tot)), dark energy (rho Lambda, w etc), the primordial density fluctuations (Q, n(s), dn(s)/d ln k etc) and primordial gravitational waves (r, n(t) etc). We compute this multivariate probability distribution for various classes of single-field slow-roll models, exploring its dependence on the characteristic inflationary energy scales, the shape of the potential V and the choice of measure underlying the calculation. We find that unless the characteristic scale Delta phi on which V varies happens to be near the Planck scale, the only aspect of V that matters observationally is the statistical distribution of its peaks and troughs. For all energy scales and plausible measures considered, we obtain the predictions Omega(tot) approximate to 1 +/- 10(-5), w = - 1 and rho(Lambda) in the observed ballpark but uncomfortably high. The high energy limit predicts n(s) approximate to 0.96, dn(s)/d ln k approximate to - 0.0006, r approximate to 0.15 and n(t) approximate to - 0.02, consistent with observational data and indistinguishable from eternal V proportional to phi(2) inflation. The low energy limit predicts five parameters but favours larger Q and redder n(s) than observed. We discuss the coolness problem, the smoothness problem and the pothole paradox, which severely limit the viable class of models and measures. Predictions insensitive to pre-inflationary conditions can arise either from eternal inflation attractor behaviour or from anthropic selection effects probing merely a tiny non-special part of the initial distribution. We argue that these two mechanisms are severely challenged by the coolness problem and the smoothness problem, respectively. Our findings bode well for detecting an inflationary gravitational wave signature with future CMB polarization experiments, with the arguably best-motivated single-field models favouring the detectable level r similar to 0.03.
Keywords:
inflation
physics of the early universe
Journal
IF:
5.9
Papers:
1.3W
Citations:
4.7W
Organization
No organization information available
Cited Papers
.png){kind=icon}
ShareSaveShareSaveEffects of sperm-reactive antibodies present in human infertile sera on fertility of female rabbits
PREAI
ShareSaveFirst-year Wilkinson Microwave Anisotropy Probe (WMAP) observations:: Implications for inflation
OAAI
OAAIShareSaveShareSave
View more