Cosmological phase transitions and evolution of topological defects

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  • English
by
University of Tokyo , [S.l.]
StatementMichiyasu Nagasawa.
ID Numbers
Open LibraryOL15418082M

On Topological Defects and Cosmological Constant. to obtain cosmological constant from the phase transitions of the early universe when topological defects, namely monopole might have existed. After an introduction to standard cosmological theory and the theory of phase transitions in the early universe, the book then describes, in turn, the properties, formation, and cosmological.

Symmetry breaking phase transitions and topological defects Spontaneous symmetry breaking Defect formation and evolution in the expanding universe. In the following section we explain how defects form during a cosmological phase Cited by: This book sheds new light on topological defects in widely differing systems, using the Velocity-Dependent One-Scale Model to better understand their evolution.

Topological defects – cosmic strings, monopoles, domain walls or others - necessarily form at cosmological (and condensed matter) phase transitions.

Details Cosmological phase transitions and evolution of topological defects FB2

PHYSICAL FOUNDATIONS OF COSMOLOGY Topological defects 5 Inflation I: homogeneous limit Problem of initial conditions According to the theory of the cosmological phase transitions, during the first 10−10 seconds after the big bang there was not.

Abstract. Evolution of the order parameter in condensed matter analogues of cosmological phase transitions is discussed.

It is shown that the density of the frozen-out topological defects is set by the competition between the quench rate - the rate at which the phase transition is taking place - and the relaxation rate of the order by: As cosmological consequences, the non-singular origin of the universe with the early evolution and resolution of problems encountered by the standard cosmology have been described in detail.

Also, an explanatory account of Lyra geometry,a modification of Riemannian geometry, together with DKP field, spinorial field and gravitational field in Cited by: 3. The first third of the book carefully develops the necessary background in general relativity and quantum fields.

The rest of the book then provides self-contained accounts of all the key topics in contemporary cosmology, including inflation, topological defects, gravitational lensing, galaxy formation, large-scale structure and the distance by:   Topological defects can play an important role in describing the properties of many condensed matter systems (e.g.

superfluids and superconduc tors); they can catalyze many unusual effects in particle physics models and they may be responsible for seeding the density perturbations in the early Universe which de velop into galaxies and the large.

Description Cosmological phase transitions and evolution of topological defects PDF

This book sheds new light on topological defects in widely differing systems, using the Velocity-Dependent One-Scale Model to better understand their evolution.

Topological defects - cosmic strings, monopoles, domain walls or others - necessarily form at cosmological (and condensed matter) phase transitions. Now in paperback, this book is the first comprehensive and coherent introduction to the role of cosmic strings and other topological defects in the universe.

This study has been one of the major driving forces in cosmology over the last decade, and lies at the fruitful intersection of particle physics and cosmology.

After an introduction to standard cosmological. This book is the first comprehensive and coherent introduction to the role of cosmic strings and other topological defects in the universe. This study has been one of the major driving forces in cosmology over the last decade, and lies at the fruitful intersection of.

Get this from a library. Defect evolution in cosmology and condensed matter: quantitative analysis with the velocity-dependent one-scale model. [C J A P Martins] -- This book sheds new light on topological defects in widely differing systems, using the Velocity-Dependent One-Scale Model to better understand their evolution.

This book is written from the viewpoint of a deep connection between cosmology and particle physics. It presents the results and ideas on both the homogeneous and isotropic Universe at the hot stage of its evolution and in later stages.

The main chapters describe in a systematic and pedagogical way. In this review we describe the formation and evolution of topological defects which may form during symmetry breaking phase transitions in the early Universe. After an introduction to cosmological perturbation theory, we discuss the scale invariant spectrum of fluctuations induced by defects in a homogeneous and isotropic by: Basic Mathematics for Astronomy (PDF 34P) This guide covers the following topics: Phase transitions in the early universe, Cosmic strings and other topological defects, Cosmic string dynamics and evolution, High-resolution cosmic string simulations, Cosmic strings and large-scale structure, Texture models and large-scale structure.

Cosmic Strings and other defects. This guide covers the following topics: Phase transitions in the early universe, Cosmic strings and other topological defects, Cosmic string dynamics and evolution, High-resolution cosmic string simulations, Cosmic strings and large-scale structure, Texture models and large-scale structure.

Topological defects have recently become of great interest in condensed matter physics, particle physics and cosmology.

They are the unavoidable remnants of many symmetry breaking phase transitions. Topological defects can play an important role in describing the properties of many condensed matter. 2 Symmetry Breaking Phase Transitions and the Formation of Topological Defects 12 Spontaneous symmetry breaking 12 Symmetry restoration at high temperature 16 Exact solutions for strings 21 General remarks on topological defects 25 Defect formation and evolution in the expanding universe 26 3 Theoretical Framework 31   Cosmic Strings and Other Topological Defects by Alex Vilenkin,available at Book Depository with free delivery worldwide.5/5(3).

Part 3 describes extensions of this model and opens up current research in the field: scalar-tensor theories, supersymmetry, the cosmological constant problem and acceleration of the universe, topology of the universe, grand unification and baryogenesis, topological defects and phase transitions, string inspired cosmology including branes and.

Cosmic strings are hypothetical 1-dimensional topological defects which may have formed during a symmetry breaking phase transition in the early universe when the topology of the vacuum manifold associated to this symmetry breaking was not simply is expected that at least one string per Hubble volume is formed.

Their existence was first contemplated by the. Part 3 describes extensions of this model and opens up current research in the field: scalar-tensor theories, supersymmetry, the cosmological constant problem and acceleration of the universe, topology of the universe, grand unification and baryogenesis, topological defects and phase transitions, string inspired cosmology including branes and.

Cosmological phase transitions Generation of baryon asymmetry Generation of dark matter Structure Formation in the Universe Before the Hot Epoch Argument from observations Drawbacks of the Hot Big Bang theory Inflationary Theory Alternatives to inflation 32Price: $   Phase Transitions in the Early Universe; This ratio stays constant at the hot stage of the cosmological evolution provided there are no processes that violate baryon number or produce large entropy.

(topological defects) or by the existence of conserved global quantum numbers (non-topological solitons, Q-balls). Of interest are both. The Kibble–Zurek mechanism (KZM) describes the non-equilibrium dynamics and the formation of topological defects in a system which is driven through a continuous phase transition at finite rate.

It is named after Tom W. Kibble, who pioneered the study of domain structure formation in the early universe, and Wojciech H. Zurek, who related the number of defects it creates to the.

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The role of topological defects in symmetry-breaking phase transitions has become a prime topic in cosmology and high-temperature superconductivity, even though direct imaging of these defects is Cited by: INFLATIONARY UNIVERSE.

Adapted from P. Coles, This also solves problems associated with the formation of monopoles and other topological defects in the early Universe, Attempts to calculate the size of the cosmological constant induced by phase transitions in this way produce enormously large values. 2 Symmetry Breaking Phase Transitions and the Formation of Topological Defects 11 Spontaneous symmetry breaking 11 Symmetry restoration at high temperature 15 Exact solutions for strings 20 General remarks on topological defects 24 Defect formation and evolution in the expanding universe 25 3 Theoretical Framework The Yang-Mills theory has gauge group SU(N), where N is very large, and it is said to be 'supersymmetric' because it has a symmetry which allows you to exchange bosons and fermions.

The hope is that this theory will eventually teach us something about QCD (quantum chromodynamics), which is a gauge theory with gauge group SU (3). Topological defects formed at symmetry-breaking phase transitions play an important role in many different fields of physics.

They appear in many condensed-matter systems at low temperature; examples include vortices in superfluid helium-4, a rich variety of defects in helium-3, quantized mag­ netic flux tubes in type-II superconductors, and disclination lines and other defects in .topological structures such as vortices and solitons in quenched cold-atom experiments has enabled the veri cation of the Kibble{Zurek mechanism predicting the density of topological defects in continuous phase transitions, rst proposed File Size: 1MB.10 Topological defects Phase transitions in cosmology Classes of topological defect Magnetic monopoles Cosmic strings and structure formation 11 Inflationary cosmology General arguments for inflation An overview of inflation Inflation field dynamics Inflation File Size: KB.