Predictions in Eternal Inflation

Winitzki, Sergei

doi:10.1007/978-3-540-74353-8_5

Cited by 64 publications

(72 citation statements)

References 151 publications

(301 reference statements)

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“…e.g. [28]), by assigning finite entropy to de Sitter space [29][30][31], or, via thoroughly incorporating the null-energy condition [32], for instance. Instead, here, the limited duration of inflation originates from the quantum resolution of the inflation as well as of the graviton condensate, which constitute the classical backgrounds in the limit of infinite N .…”

Section: Competing Fluctuationsmentioning

confidence: 99%

Corpuscular consideration of eternal inflation

Kühnel

Sandstad

2015

Eur. Phys. J. C

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We review the paradigm of eternal inflation in the light of the recently proposed corpuscular picture of spacetime. Comparing the strength of the average fluctuation of the field up its potential with that of quantum depletion, we show that the latter can be dominant. We then study the full respective distributions in order to show that the fraction of the space-time which has an increasing potential is always below the eternal-inflation threshold. We prove that for monomial potentials eternal inflaton is excluded. This is likely to hold for other models as well.

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Section: Competing Fluctuationsmentioning

confidence: 99%

Corpuscular consideration of eternal inflation

Kühnel

Sandstad

2015

Eur. Phys. J. C

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“…[8,9,70] for a review). The large-scale structure of the universe then consists of many causally disconnected regions in which different vacua might be physically realized, but where there is always a spatial slicing along which part of the universe remains in the false vacuum.…”

Section: Eternal Inflation and The Landscapementioning

confidence: 99%

Field dynamics and tunneling in a flux landscape

Johnson

Larfors

2008

Phys. Rev. D

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We investigate field dynamics and tunneling between metastable minima in a landscape of Type IIB flux compactifications, utilizing monodromies of the complex structure moduli space to continuously connect flux vacua. After describing the generic features of a flux-induced potential for the complex structure and Type IIB axio-dilaton, we specialize to the Mirror Quintic Calabi-Yau to obtain an example landscape. Studying the cosmological dynamics of the complex structure moduli, we find that the potential generically does not support slow-roll inflation and that in general the landscape separates neatly into basins of attraction of the various minima. We then discuss tunneling, with the inclusion of gravitational effects, in many-dimensional field spaces. A set of constraints on the form of the Euclidean paths through field space are presented, and then applied to construct approximate instantons mediating the transition between de Sitter vacua in the flux landscape. We find that these instantons are generically thick-wall and that the tunneling rate is suppressed in the large-volume limit. We also consider examples where supersymmetry is not broken by fluxes, in which case near-BPS thin-wall bubbles can be constructed. We calculate the bubble wall tension, finding that it scales like a D-or NS-brane bubble, and comment on the implications of this correspondence. Finally, we present a brief discussion of eternal inflation in the flux-landscape.

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“…The results of some of these methods are not sensitive to the choice of time parametrization, but they do depend on the choice of the cut-off. A detailed discussion of this series of proposals can be found in [190,197,198].…”

Section: Brane Inflationmentioning

confidence: 99%

Inflationary cosmology

Abbott¹

2004

Cosmology in Gauge Field Theory and String Theory

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I give a general review of the history of inflationary cosmology and of its present status. Contents Brief history of inflationSince inflationary theory is now more than 25 years old, perhaps it is not inappropriate to start this paper with a brief history of the first stages of its development.Several ingredients of inflationary cosmology were discovered in the beginning of the 70's. The first realization was that the energy density of a scalar field plays the role of the vacuum energy/cosmological constant [1], which was changing during the cosmological phase transitions [2]. In certain cases these changes occur discontinuously, due to first order phase transitions from a supercooled vacuum state (false vacuum) [3].In 1978, Gennady Chibisov and I tried to use these facts to construct a cosmological model involving exponential expansion of the universe in the supercooled vacuum as a source of the entropy of the universe, but we immediately realized that the universe becomes very inhomogeneous after the bubble wall collisions. I mentioned our work in my review article [4], but did not pursue this idea any further.The first semi-realistic model of inflationary type was proposed by Alexei Starobinsky in 1979Starobinsky in -1980. It was based on investigation of a conformal anomaly in quantum gravity. His model was rather complicated, and its goal was somewhat different from the goals of inflationary cosmology. Instead of attempting to solve the homogeneity and isotropy problems, Starobinsky considered the model of the universe which was homogeneous and isotropic from the very beginning, and emphasized that his scenario was "the extreme opposite of Misner's initial chaos."On the other hand, Starobinsky's model did not suffer from the graceful exit problem, and it was the first model predicting gravitational waves with a flat spectrum [5]. The first mechanism of production of adiabatic perturbations of the metric with a flat spectrum, which are responsible for galaxy production, and which were found by the observations of the CMB anisotropy, was proposed by Mukhanov and Chibisov [6] in the context of this model.A much simpler inflationary model with a very clear physical motivation was proposed by Alan Guth in 1981 [7]. His model, which is now called "old inflation," was based on the theory of supercooling during the cosmological phase transitions [3]. Even though this scenario did not work, it played a profound role in the development of inflationary cosmology since it contained a very clear explanation how inflation may solve the major cosmological problems.According to this scenario, inflation is as exponential expansion of the universe in a supercooled false vacuum state. False vacuum is a metastable state without any fields or particles but with large energy density. Imagine a universe filled with such "heavy nothing." When the universe expands, empty space remains empty, so its energy density does not change. The universe with a constant energy density expands exponentially, thus we have inflation in...

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Predictions in Eternal Inflation

Cited by 64 publications

References 151 publications

Corpuscular consideration of eternal inflation

Corpuscular consideration of eternal inflation

Field dynamics and tunneling in a flux landscape

Inflationary cosmology

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