• Documents
  • Authors
  • Tables
  • Log in
  • Sign up
  • MetaCart
  • Donate

CiteSeerX logo

Advanced Search Include Citations
Advanced Search Include Citations | Disambiguate

Elementary Particle Physics and Inflationary Cosmology (Nauka, (1990)

by A D Linde
Add To MetaCart

Tools

Sorted by:
Results 1 - 10 of 821
Next 10 →

Particle physics model of inflation and the cosmological density perturbation

by David H. Lyth, Antonio Riotto
"... This is a review of models of inflation, and their predictions for the primordial curvature perturbation that is thought to be the origin of structure in the Universe. The spectral index n, specifying the scale-dependence of the spectrum of the curvature perturbation, will be a powerful discriminato ..."
Abstract - Cited by 163 (7 self) - Add to MetaCart
This is a review of models of inflation, and their predictions for the primordial curvature perturbation that is thought to be the origin of structure in the Universe. The spectral index n, specifying the scale-dependence of the spectrum of the curvature perturbation, will be a powerful discriminator between models, when it is measure with accuracy ∆n ∼ 0.01. The usual formula for n is derived, as well as its less familiar extension to the case of a multi-component inflaton; in both cases the key ingredient is the separate evolution of causally disconnected regions of the Universe. Primordial gravitational waves will be an even more powerful discriminator if they are observed, since most models of inflation predict that they are completely negligible. We focus on the new wave of models, which are firmly rooted in modern particle theory and have supersymmetry as a crucial ingredient. The essential particle theory background is summarized, first at an elementary level and later at a more advanced one. The review is addressed to both astrophysicists and particle physicists, and each section is fairly homogeneous regarding the assumed background knowledge.
(Show Context)

Citation Context

...reaking 129 31 Introduction We do not know the history of the observable Universe before the epoch of nucleosynthesis, but it is widely believed that there was an early era of cosmological inflation =-=[192, 167, 184, 185]-=-. During this era, the Universe was filled with a homogeneous scalar field φ, called the inflaton field, and essentially nothing else. The potential V (φ) dominated the energy density of the Universe,...

The holographic principle

by Raphael Bousso - Rev. Mod. Phys , 2002
"... There is strong evidence that the area of any surface limits the information content of adjacent spacetime regions, at 1.4 ×10 69 bits per square meter. We review the developments that have led to the recognition of this entropy bound, placing special emphasis on the quantum properties of black hole ..."
Abstract - Cited by 132 (9 self) - Add to MetaCart
There is strong evidence that the area of any surface limits the information content of adjacent spacetime regions, at 1.4 ×10 69 bits per square meter. We review the developments that have led to the recognition of this entropy bound, placing special emphasis on the quantum properties of black holes. The construction of light-sheets, which associate relevant spacetime regions to any
(Show Context)

Citation Context

...VII.A.3, VII.B).—Davies (1987) obtained w ≥ −1 as a condition for the growth of the apparent horizon in an inflating universe.33 According to the inflationary model of the early universe (see, e.g., =-=Linde, 1990-=-), a different non-adiabatic process occurred at the end of inflation. At the time of reheating, matter is produced and a large amount of entropy is generated. One might be concerned that the holograp...

Electroweak baryon number nonconservation in the early universe and in highenergy collisions,”Uspekhi

by V A Rubakov, M E Shaposhnikov - Fizicheskikh Nauk, , 1996
"... ..."
Abstract - Cited by 113 (3 self) - Add to MetaCart
Abstract not found
(Show Context)

Citation Context

...he so-called infrared problem in thermodynamics of the gauge fields. There are many excellent reviews and books devoted to the study of the phase transitions in gauge theories, see, for instance ref. =-=[118, 119, 120, 121]-=-. Our purpose in this section is to report on the progress that was achieved in this area in the last few years. Our special interest is in the study of the first order phase transitions which are str...

The pre-big bang scenario in string cosmology

by M. Gasperini, G. Veneziano - Phys. Rept , 2003
"... We review physical motivations, phenomenological consequences, and open problems of the so-called pre-big bang scenario in superstring cosmology. Contents 1 ..."
Abstract - Cited by 89 (3 self) - Add to MetaCart
We review physical motivations, phenomenological consequences, and open problems of the so-called pre-big bang scenario in superstring cosmology. Contents 1
(Show Context)

Citation Context

... as another great success of general relativity, was later discovered to suffer from huge fine-tuning problems. Some of these conceptual problems are solved by the standard inflationary paradigm (see =-=[441, 420]-=- for a review), yet inflation remains a generic idea in search of a theory that will embody it naturally. Furthermore, the classical theory of inflation does not really address the problem of how the ...

Towards inflation in string theory

by Shamit Kachru, Renata Kallosh, Andrei Linde, Juan Maldacena , Liam McAllister, Sandip P. Trivedi - JCAP , 2003
"... We investigate the embedding of brane inflation into stable compactifications of string theory. At first sight a warped compactification geometry seems to produce a naturally flat inflaton potential, evading one well-known difficulty of brane-antibrane scenarios. Careful consideration of the closed ..."
Abstract - Cited by 82 (9 self) - Add to MetaCart
We investigate the embedding of brane inflation into stable compactifications of string theory. At first sight a warped compactification geometry seems to produce a naturally flat inflaton potential, evading one well-known difficulty of brane-antibrane scenarios. Careful consideration of the closed string moduli reveals a further obstacle: superpotential stabilization of the compactification volume typically modifies the inflaton potential and renders it too steep for inflation. We discuss the non-generic conditions under which this problem does not arise. We conclude that brane inflation models can only work if restrictive assumptions about the method of volume stabilization, the warping of the internal space, and the source of inflationary energy are satisfied. We argue that this may not be a real problem, given the large range of available fluxes and background geometries in string theory.
(Show Context)

Citation Context

... of initial conditions: Why should the field φ start in the particular slow-roll domain? For the simplest chaotic inflation models of the type of m2 2 φ2 this problem can be easily resolved, see e.g. =-=[103]-=-. The problem of initial conditions in the theories where inflation is possible only at the densities much smaller than the Planck density is much more complicated; for a possible solution see e.g. [1...

Metric-affine f(R) theories of gravity

by Thomas P. Sotiriou, Valerio Faraoni - J. Suppl. Ser , 2007
"... Modified gravity theories have received increased attention lately due to combined motivation coming from high-energy physics, cosmology and astrophysics. Among numerous alternatives to Einstein’s theory of gravity, theories which include higher order curvature invariants, and specifically the parti ..."
Abstract - Cited by 69 (1 self) - Add to MetaCart
Modified gravity theories have received increased attention lately due to combined motivation coming from high-energy physics, cosmology and astrophysics. Among numerous alternatives to Einstein’s theory of gravity, theories which include higher order curvature invariants, and specifically the particular class of f(R) theories, have a long history. In the last five years there has
(Show Context)

Citation Context

..., contrary to past expectations. 1 Note that this late time speed-up comes to be added to an early time accelerated epoch as predicted by the inflationary paradigm (Guth, 1981; Kolb and Turner, 1992; =-=Linde, 1990-=-). The inflationary epoch is needed to address the so-called horizon, flatness and monopole problems (Kolb and Turner, 1992; Linde, 1990; Misner, 1968; Weinberg, 1972), as well as to provide the mecha...

Computational capacity of the universe

by Seth Lloyd - Physical Review Letters
"... Merely by existing, all physical systems register information. And by evolving dynamically in time, they transform and process that information. The laws of physics determine the amount of information that a physical system can register (number of bits) and the number of elementary logic operations ..."
Abstract - Cited by 55 (0 self) - Add to MetaCart
Merely by existing, all physical systems register information. And by evolving dynamically in time, they transform and process that information. The laws of physics determine the amount of information that a physical system can register (number of bits) and the number of elementary logic operations that a system can perform (number of ops). The universe is a physical system. This paper quantifies the amount of information that the universe can register and the number of elementary operations that it can have performed over its history. The universe can have performed no more than 10 120 ops on 10 90 bits. ‘Information is physical ’ 1. This statement of Landauer has two complementary interpretations. First, information is registered and processed by physical systems. Second, all physical systems register and process information. The description of physical systems in terms of information and information processing is complementary to the conventional description of physical system in terms of the laws of physics. A recent paper by the author2 put bounds on the amount of information processing that can be performed by physical systems. The first limit is on speed. The Margolus/Levitin theorem3 implies that the total

The stochastic gravity–wave background: sources and detection

by B. Allen
"... ..."
Abstract - Cited by 51 (11 self) - Add to MetaCart
Abstract not found
(Show Context)

Citation Context

...r general interest, these three examples serve to motivate a number of interesting observations and comments. The first model we examine is the standard “inflationary” scenario for the early universe =-=[17, 33]-=-. In this model, as the universe cooled, it passed through a phase in which the energy-density of the universe was dominated by vacuum energy, and the scale factor increased exponentially-rapidly. You...

The Cosmological Constant and the String Landscape

by Joseph Polchinski
"... Theories of the cosmological constant fall into two classes, those in which the vacuum energy is fixed by the fundamental theory and those in which it is adjustable in some way. For each class we discuss key challenges. The string theory landscape is an example of an adjustment mechanism. We discuss ..."
Abstract - Cited by 49 (1 self) - Add to MetaCart
Theories of the cosmological constant fall into two classes, those in which the vacuum energy is fixed by the fundamental theory and those in which it is adjustable in some way. For each class we discuss key challenges. The string theory landscape is an example of an adjustment mechanism. We discuss the status of this idea, and future directions. Rapporteur talk at the 23rd Solvay Conference in Physics, December, 2005. 1 The cosmological constant I would like to start by drawing a parallel to an earlier meeting — not a Solvay conference, but the 1947 Shelter Island conference. In both cases a constant of nature was at the center of discussions. In each case theory gave an unreasonably large or infinite value for the constant, which had therefore been assumed to vanish for reasons not yet understood, but in each case experiment or observation had recently found a nonzero value. At Shelter

Large Scale Structure And Supersymmetric Inflation Without Fine Tuning,” Phys

by G. Dvali, Q. Shafi, R. Schaefer - Rev. Lett , 1994
"... We explore constraints on the spectral index n of density fluctuations and the neutrino energy density fraction ΩHDM, employing data from a variety of large scale observations. The best fits occur for n ≈ 1 and ΩHDM ≈ 0.15 − 0.30, over a range of Hubble constants 40 − 60 km s −1 Mpc −1. We present a ..."
Abstract - Cited by 48 (0 self) - Add to MetaCart
We explore constraints on the spectral index n of density fluctuations and the neutrino energy density fraction ΩHDM, employing data from a variety of large scale observations. The best fits occur for n ≈ 1 and ΩHDM ≈ 0.15 − 0.30, over a range of Hubble constants 40 − 60 km s −1 Mpc −1. We present a new class of inflationary models based on realistic supersymmetric grand unified theories which do not have the usual ‘fine tuning ’ problems. The amplitude of primordial density fluctuations, in particular, is found to be proportional to (MX/MP) 2, where MX(MP) denote the GUT (Planck) scale, which is reminiscent of cosmic strings! The spectral index n = 0.98, in excellent agreement with the observations provided the dark matter is a mixture of ‘cold’ and ‘hot ’ components. PACS Nos: 98.80Cq, 98.65Dx, 12.10Dm, 11.30Pb 1 Recent studies of large scale structure formation [1], when confronted with
(Show Context)

Citation Context

...scale structure formation [1], when confronted with a variety of data from the Cosmic Background Explorer [2] (COBE) and other large scale galaxy surveys, provide support for an inflationary scenario =-=[3]-=- in which the spectral index of density fluctuations n is close to unity and the dark matter is a mixture of cold and hot components. Non-supersymmetric grand unified theories which give rise to preci...

Powered by: Apache Solr
  • About CiteSeerX
  • Submit and Index Documents
  • Privacy Policy
  • Help
  • Data
  • Source
  • Contact Us

Developed at and hosted by The College of Information Sciences and Technology

© 2007-2016 The Pennsylvania State University