How Many e-Folds Should We Expect from High-Scale Inflation?

  title={How Many e-Folds Should We Expect from High-Scale Inflation?},
  author={Grant N. Remmen and S. Carroll},
  journal={Physical Review D},
We address the issue of how many e-folds we would naturally expect if inflation occurred at an energy scale of order 10^(16) GeV. We use the canonical measure on trajectories in classical phase space, specialized to the case of flat universes with a single scalar field. While there is no exact analytic expression for the measure, we are able to derive conditions that determine its behavior. For a quadratic potential V(ϕ)=m^2ϕ^2/2 with m=2×10^(13) GeV and cutoff at M_(Pl)=2.4×10^(18) GeV, we… 

Figures from this paper

Natural inflation, strong dynamics, and the role of generalized anomalies

We revisit models of natural inflation and show that the single-field effective theory described by the potential $V(a)\sim \cos\frac{a}{f}$ breaks down as the inflaton $a$ makes large-field

Can CMB data constrain the inflationary field range?

We study to what extent the spectral index ns and the tensor-to-scalar ratio r determine the field excursion Δϕ during inflation. We analyse the possible degeneracy of Δ ϕ by comparing three broad

Finite inflation in curved space

We investigate the effects of non-zero spatial curvature on cosmic inflation in the light of cosmic microwave background (CMB) anisotropy measurements from the Planck 2018 legacy release and from the

Global dynamics and inflationary center manifold and slow-roll approximants

We consider the familiar problem of a minimally coupled scalar field with quadratic potential in flat Friedmann-Lemaitre-Robertson-Walker cosmology to illustrate a number of techniques and tools,

Theoretical considerations in the use of scalar-tensor theories of gravity in inflationary models

The inflationary paradigm is one which was designed to answer questions that arose from classical Hot Big Bang cosmology. The period of rapid expansion in the early Universe provides a mechanism to

S -dual inflation and the string swampland

The swampland de Sitter conjecture in combination with upper limits on the tensor-to-scalar ratio r derived from observations of the cosmic microwave background endangers the paradigm of slow-roll

Viability of slow-roll inflation in light of the non-zero kmin measured in the cosmic microwave background power spectrum

Slow-roll inflation may simultaneously solve the horizon problem and generate a near scale-free fluctuation spectrum P(k). These two processes are intimately connected via the initiation and duration

Flows into inflation: An effective field theory approach

We analyze the flow into inflation for generic "single-clock" systems, by combining an effective field theory approach with a dynamical-systems analysis. In this approach, we construct an expansion

How decoherence affects the probability of slow-roll eternal inflation

Slow-roll inflation can become eternal if the quantum variance of the inflaton field around its slowly rolling classical trajectory is converted into a distribution of classical spacetimes inflating

Effective field theories as a novel probe of fine-tuning of cosmic inflation

  • Feraz Azhar
  • Economics
    Studies in History and Philosophy of Science Part B: Studies in History and Philosophy of Modern Physics
  • 2020



BICEP2 Collaboration)

  • Phys. Rev. Lett. 112,
  • 2014

I and J


  • Rev. D 88, 083518
  • 2013

Planck Collaboration) (2013), arXiv:1303.5076 [astro-ph.CO

  • 2013


  • Phys. B281, 736
  • 1987


  • Rev. Lett. 85, 3572
  • 2000


  • Rev. D 77, 063516
  • 2008

and T

  • Yanagida, Phys.Rev.Lett. 85, 3572
  • 2000


  • Rev. Lett. 65, 3233
  • 1990


  • Rev. D 90, 041303 (2014). GRANT N. REMMEN AND SEAN M. CARROLL PHYSICAL REVIEW D 90, 063517
  • 2014