Origin of density fluctuations in extended inflation

Cover of: Origin of density fluctuations in extended inflation | Edward W. Kolb

Published by Fermi National Accelerator Laboratory, National Aeronautics and Space Administration, National Technical Information Service, distributor in Batavia, Ill, [Washington, DC, Springfield, Va .

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  • Inflationary universe.

Edition Notes

Book details

StatementEdward W. Kolb, David S. Salopek, and Michael S. Turner.
SeriesNASA contractor report -- NASA CR-182852.
ContributionsSalopek, David S., Turner, Michael Stanley., United States. National Aeronautics and Space Administration.
The Physical Object
Pagination1 v.
ID Numbers
Open LibraryOL15397979M

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The density fluctuations (both curvature and isocurvature) that arise due to quantum fluctuations in a simple model of extended inflation based upon the Jordan-Brans-Dicke theory are calculated.

Get this from a library. Origin of density fluctuations in extended inflation. [Edward W Kolb; David S Salopek; Michael Stanley Turner; United States. National Aeronautics and Space Administration.]. Abstract.

In that talk I presented some work by Carsten Gundlach, David Langlois, David Polarski and myself showing how a spectrum of density fluctuations, relevant for galaxy formation, can be derived from vacuum density fluctuations, which are produced and amplified in an early period of extended inflation of the early : Nathalie Deruelle.

We analyse the implications for inflationary models of the cosmic microwave background (cmb) anisotropy measured by COBE.

Vacuum fluctuations during inflation generate an adiabatic density perturbation, and also gravitational waves. The ratio of these two contributions to the cmb anisotropy is given for an arbitrary slow-roll inflaton potential.

Results from the IRAS/QDOT and Cited by: This is precisely the origin of the density and gravity-wave fluctuations in inflation. Modes at short wavelengths are rapidly redshifted by the inflationary expansion so that the wavelength of the mode is larger than the horizon size, Eq. Kolb, D. Salopek and M.

Turner, “Origin of Density Fluctuations Origin of density fluctuations in extended inflation book Extended Inflation”, Fermilab preprint () Google Scholar [24] E.

Copeland, E. Kolb and A. Liddle, Phys Rev D 42 () ADS CrossRef Google Scholar. Density fluctuations from inflation. So far we have seen that the standard FRW cosmology has two (related) unexplained issues: why is the universe so flat and why is it so smooth.

These questions are difficult to answer in the context of a matter- or radiation-dominated cosmology without resorting to simply setting the initial conditions of the. The fluctuations in the CMB you refer to are over-densities and under-densities in the matter distribution of the early universe (among other things).

An over-density is where a region of space has a more dense distribution of matter than the average value of the rest of space. Quite literally, the density is over the background value. Inflation predicted that these fluctuations should have been % adiabatic, which should leave unique signatures in both the cosmic microwave.

Inflation is when most prices in an entire economy are rising. But there is an extreme form of inflation called hyperinflation. This occurred in Germany between andand more recently in Zimbabwe between and In November ofZimbabwe had an inflation rate of billion percent.

In physical cosmology, cosmic inflation, cosmological inflation, or just inflation, is a theory of exponential expansion of space in the early inflationary epoch lasted from 10 −36 seconds after the conjectured Big Bang singularity to Origin of density fluctuations in extended inflation book time between 10 −33 and 10 −32 seconds after the singularity.

Following the inflationary period, the universe continued to expand, but at. Inflation History and the Sacrifice Ratio: Episode-Specific Evidence By Senda, Takashi; Smith, Julie K Contemporary Economic Policy, Vol. 26, No. 3, July PR PEER-REVIEWED PERIODICAL Peer-reviewed publications on Questia are publications containing articles which were subject to evaluation for accuracy and substance by professional peers of.

Density perturbations arising out of the quantum fluctuations in a Brans-Dicke field in the context of extended inflation have been studied. We have used a model in which the Brans-Dicke parameter varies with time.

We find that the density perturbations are large in magnitude and have a scale invariant spectrum. The primordial density perturbation: cosmology, inflation and the origin of structure David H.

Lyth, Andrew R. Liddle This graduate-level textbook gives a thorough account of theoretical cosmology and perturbations in the early Universe, describing their observational consequences and showing how to relate such observations to primordial.

Monetary Regimes and Inflation: History, Economic and Political Relationships, Second Edition Peter Bernholz. out of 5 stars 1. Paperback. $ Only 19 left in stock (more on the way). The Great Inflation and Its Aftermath: The Past and Future of American Affluence Robert J.

Reviews: 4. Field fluctuations. A quantum fluctuation is the temporary appearance of energetic particles out of empty space, as allowed by the uncertainty uncertainty principle states that for a pair of conjugate variables such as position/momentum or energy/time, it is impossible to have a precisely determined value of each member of the pair at the same time.

[+] inflation ends, they become density fluctuations. This leads, over time, to the large-scale structure in the Universe today, as well as the fluctuations in temperature observed in the CMB. Inflation within a single bubble can create a smooth Universe with a hyperbolic geometry, just as is required for a Universe of subcritical density.

Single bubble open inflation, based on ideas of S. Coleman and F. de Luccia and of J.R. Gott, III, in the early s, was further developed in the mids by M. Bucher, A.S.

Goldhaber, and N. Accordingly, we derive the modifications in the Friedmann equations due to single scalar field potentials describing power-law and minimal-supersymmetrically extended inflation. By implementing four types of the equations-of-state charactering the cosmic background geometry, the dependence of the tensorial and spectral density fluctuations and.

terms as in k-inflation or DBI inflation, models with general higher-derivative interactions of the inflaton field such as ghost inflation, and models arising from effective field theories n Folded NG, e.g.

single-field models w non-Bunch-Davies vacuum, and models with general higher derivative interactions. These quantum fluctuations, which translate into density fluctuations, should be adiabatic. Fluctuations could have come in different types: adiabatic, isocurvature, or a.

The ability to reproduce the observed matter power spectrum P (k) to high accuracy is often considered as a triumph of inflation.

In this work, we explore an alternative explanation for the power spectrum based on nonperturbative quantum field-theoretical methods applied to Einstein’s gravity, instead of ones based on inflation models. In particular, the power spectral index, which.

Inflation is driven by one or more scalar fields with an appropriate potential. In this thesis we develop an analytical formalism to describe the generation of density fluctuations during inflation with multiple scalar fields.

We allow these fields to live on a non-trivial (curved) field manifold, as is often the case in high-energy theories. At the same time, the universe would be the blow-up of a region so small that fluctuations in temperature and density would be very small, explaining its smoothness.

Cosmologists soon reckoned that inflation, while creating a very uniform universe, would also explain why and how the early cosmos would be lumpy enough that the stars and galaxies.

The origin of the universe 20 Acknowledgments 21 References 21 I. THE ORIGIN OF INFLATIONARY FLUCTUATIONS Since the topic of inflation and density perturbations pretty much came to fruition at the Nuffield Workshop [15] almost 20 years ago, and since I was one of the attendees, I.

Inflation—the general rise in the prices of goods and services—is one of the differentiating characteristics of the U.S. economy in the post-World War II era. Except for, and. Inflation and Quantum Cosmology discusses the inflationary universe scenario, including the problems of the standard big bang theory and the interplay between elementary-particle theory and cosmology.

a model of an inflationary universe, through a casual mechanism, can predict energy density fluctuations leading to the formation of galaxies. The CMBR has its origin as the light which is liberated by the universe's newfound transparency at this epoch, and so measurements of its temperature fluctuations, δT/T ~ 10 −5, provide direct information about the size of primordial density fluctuations in.

Request PDF | Minimal-supersymmetric extended inflation field in Horava-Lifshitz gravity | We study the Friedmann inflation in general covariant Horava-Lifshitz (HL) gravity without the.

For cold dark energy EoS ω = − 1 / 3, we find that the tensorial-to-spectral density fluctuations are not depending on the different theories of gravity and the results are very small relative to the recent BICEP2/Keck Array-Planck observations, 1 0 − 9 ⪅ r ⪅ 1 0 − 3.

We have also calculated the tensorial and scalar perturbations of. Inflation theory says that in a slow expansion of the universe, quantum fluctuations were only on the tiny distance scales; when the universe experienced a brief period of inflation, however, these quantum fluctuations are "stretched" much larger to cause density fluctuations.

The places of higher density later caused matter to clump in those. @article{osti_, title = {Scale-invariant curvature fluctuations from an extended semiclassical gravity}, author = {Pinamonti, Nicola and INFN Sezione di Genova, Via Dodecan Genova and Siemssen, Daniel}, abstractNote = {We present an extension of the semiclassical Einstein equations which couple n-point correlation functions of a stochastic Einstein tensor to the n-point.

Sean M. Carroll (–) researched dark energy, general relativity, and spontaneous inflation; Gennady V. Chibisov (–) origin of cosmological density perturbations from quantum fluctuations; Peter Coles (–) modeled galactic clustering and authored several cosmology books. We show that when the quantum to classical transition is properly treated, with due consideration of the relation of decoherence, noise, fluctuation and dissipation, the amplitude of density contrast predicted falls in the acceptable range without requiring a fine tuning of the coupling constant of the inflation.

Inflation also forms the context for the next alternative to arise: the Chaotic Inflationary Model. One of the most fertile of the inflation theorists has been the Russian cosmologist Andrei Linde.

[33] In Linde's model inflation never ends: each inflating domain of the universe when it reaches a certain volume gives rise via inflation to. In this scenario the major part of the physical volume of the universe always remains in the inflationary phase.

During inflation the universe becomes divided into many exponentially large domains, inside which all possible metastable vacuum states and all possible types of compactification compatible with inflation are realized. Inflation is an attempt to answer that question, to say what "banged," and what drove the universe into this period of enormous expansion.

Inflation does that very wonderfully. It explains not only what caused the universe to expand, but also the origin of essentially all the matter in the universe at the same time.

The Hubble expansion rate is kilometers per second per megaparsec (to an accuracy of ). Results are consistent with inflation: W=1 to within 10%, and the spectrum of density fluctuations is the predicted one within experimental errors. The earlier 20th-century simple picture of our world as a de-accelerating, expanding Universe driven.

The book includes more than ninety figures as well as a five-page update discussing recent developments such as the COBE results. Gravitational couplings of the inflaton in extended inflation by Richard Holman Origin of density fluctuations in extended inflation by Edward W Kolb.

The density of matter was huge then -- 10 to the 94 grams (10^94) per cubic centimeter, as compared with the density of an atomic nucleus today, which is only 10 to the 14 grams (10^14). Fluctuations in the inflaton field — the field that provides the energy density to drive the expansion — become physically manifested as perturbations in the curvature once they’ve reached.The cosmic microwave background is a faint glow of light left over from the Big Bang.

It fills the entire sky and records the Universe's early history. Two independent experts outline what we know.Please leave anonymous comments for the current page, to improve the search results or fix bugs with a displayed article!

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