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  • 1
    Online Resource
    Online Resource
    Oxford :Oxford University Press, Incorporated,
    Keywords: Renormalization group. ; Critical phenomena (Physics). ; Mathematical physics. ; Electronic books.
    Description / Table of Contents: The successful calculation of critical exponents for continuous phase transitions is one of the main achievements of theoretical physics over the last quarter-century. This was achieved through the use of scaling and field-theoretic techniques which have since become standard equipment in many areas of physics, especially quantum field theory. This book provides a thorough introduction to these techniques. Continuous phase transitions are introduced, then the necessary statistical mechanics is summarized, followed by standard models, some exact solutions and techniques for numerical simulations. The real-space renormalization group and mean-field theory are then explained and illustrated. The final chapters cover the Landau-Ginzburg model, from physical motivation, through diagrammatic perturbation theory and renormalization to therenormalization group and the calculation of critical exponents above and below the critical temperature.
    Type of Medium: Online Resource
    Pages: 1 online resource (477 pages)
    Edition: 1st ed.
    ISBN: 9780191660566
    DDC: 530.1/2
    Language: English
    Note: Cover -- Contents -- 1 Introduction -- 1.1 Continuous phase transitions and critical points -- 1.1.1 Divergences and critical exponents -- 1.1.2 Fluctuations and critical opalescence -- 1.2 The order parameter -- 1.2.1 Liquid-gas transition -- 1.2.2 Binary fluids -- 1.2.3 Ferromagnetic/paramagnetic transition -- 1.2.4 Anti-ferromagnetic/paramagnetic transition -- 1.2.5 Helium I/helium II transition -- 1.2.6 Conductor/superconductor transitions -- 1.2.7 Helium three -- 1.3 Correlation functions -- 1.4 Universality -- 1.5 Thermodynamic potentials -- 1.5.1 The Widom and Kadanoff scaling hypotheses -- 1.6 Why study phase transitions? -- Problems -- 2 Statistical mechanics -- 2.1 Thermodynamic quantities -- 2.2 Fluctuations and correlation functions -- 2.3 Metastability and spontaneous symmetry breaking -- 2.3.1 Metastability -- 2.3.2 Spontaneous symmetry breaking -- Problems -- 3 Models -- 3.1 Description of models -- 3.1.1 The Ising model -- 3.1.2 The lattice gas -- 3.1.3 ß-brass -- 3.1.4 The XY and Heisenberg models -- 3.1.5 Potts model -- 3.1.6 Gaussian and spherical models -- 3.1.7 Percolation model -- 3.2 Transfer matrices and the Ising ring -- 3.2.1 Solution of the Ising ring -- 3.2.2 Correlation functions -- 3.3 The partition function of the spherical model -- 3.4 High-temperature expansions and the Ising model -- 3.4.1 High-temperature expansions -- 3.4.2 The partition function of the Ising model -- 3.4.3 The correlation functions of the Ising model -- 3.4.4 Numerical evaluation of high-temperature expansions -- Problems -- 4 Numerical simulations -- 4.1 Direct evaluation of thermal averages -- 4.2 Sampling configurations -- 4.2.1 Importance sampling -- 4.2.2 General structure of numerical algorithms -- 4.3 Monte Carlo methods -- 4.3.1 The Metropolis algorithm -- 4.4 Molecular dynamics -- 4.4.1 Ergodicity and integrability. , 4.4.2 From microcanonical to canonical averages -- 4.5 Langevin equations -- 4.5.1 Comparison of the Langevin and molecular-dynamics methods -- 4.6 Independence of configurations -- 4.6.1 Correlations along the path -- 4.6.2 Critical slowing down -- 4.6.3 The Swendsen-Wang algorithm -- 4.6.4 The Wolff algorithm -- 4.7 Calculation of critical exponents from simulations -- Problems -- 5 Real-space renormalization -- 5.1 Renormalizing the lattice -- 5.2 Block variables -- 5.3 The renormalization of the Hamiltonian -- 5.3.1 Fixed points -- 5.3.2 The calculation of v -- 5.4 The renormalization of B, M, X and G[sub(c)] -- 5.4.1 The value of ω -- 5.4.2 Non-zero external field -- 5.4.3 The renormalization of M, χ and G[sub(c)] -- 5.4.4 Critical exponents for the renormalized model -- 5.5 The critical exponents for T = T[sub(c)] -- 5.5.1 The exponent η -- 5.5.2 The exponent δ -- 5.6 The critical exponents for T ≠ T[sub(c)] -- 5.6.1 The exponent β -- 5.6.2 The exponent γ -- 5.6.3 The exponent α -- 5.7 The scaling laws -- 5.8 Bond percolation in two dimensions -- 5.9 The Ising model -- 5.10 Monte Carlo renormalization -- Problems -- 6 Mean-field theory -- 6.1 Mean-field theory of the Ising model -- 6.2 Mean-field theory of percolation -- 6.3 Mean-field theory of the non-ideal gas -- 6.4 A variational derivation of mean-field theory -- 6.5 Correlation functions in mean-field theory -- 6.6 Infinite-range interactions -- 6.7 Critical exponents in mean-field theory -- 6.7.1 Calculating η from G[sup(2)][sub(c)](k) -- 6.8 What is missing from mean-field theory? -- Problems -- 7 The Landau-Ginzburg model -- 7.1 Formulation of the Landau-Ginzburg model -- 7.2 Landau theory -- Problems -- 8 Diagrammatic perturbation theory -- 8.1 The Gaussian partition function -- 8.1.1 Correlation functions in the Gaussian model. , 8.2 The partition function for the full Landau-Ginzburg model -- 8.2.1 The Feynman rules -- 8.2.2 The symmetry factor -- 8.3 The Helmholtz free energy of the Landau-Ginzburg model -- 8.3.1 Feynman rules in wavevector space -- 8.3.2 Vertex functions -- 8.4 The Gibbs free energy of the Landau-Ginzburg model -- 8.4.1 The rules for finding Γ[φ] -- 8.4.2 The loop expansion -- 8.4.3 The one-loop Gibbs free energy -- Problems -- 9 Renormalization -- 9.1 Mass renormalization -- 9.2 Field renormalization -- 9.3 Renormalizing the coupling constant -- 9.4 Renormalization at higher orders -- 9.5 More on field renormalization -- 9.6 The Ginzburg criterion -- Problems -- 10 The calculation of critical exponents for T ≥ Tc -- 10.1 Ultraviolet and infrared divergences -- 10.2 The calculation of γ -- 10.2.1 d = 4 and above -- 10.2.2 Below four dimensions -- 10.3 The calculation of η -- 10.3.1 d = 4 and above -- 10.3.2 Below four dimensions -- 10.4 The ε-expansion -- 10.4.1 Dimensional regularization -- 10.4.2 Calculating γ by dimensional regularization -- 10.4.3 Calculating η by dimensional regularization -- 10.4.4 Feynman parameters -- 10.4.5 The calculation of η again -- 10.4.6 Calculation of η by the ε-expansion -- Problems -- 11 The renormalization group -- 11.1 The renormalization group at T = T[sub(c)] -- 11.2 The exponents η and δ -- 11.2.1 The exponent η -- 11.2.2 The exponent δ -- 11.3 The calculation of β and γ[sub(1)] -- 11.3.1 The calculation of γ[sub(1)] to order ε[sup(2)] -- Problems -- 12 The renormalization group at T ≠ T[sub(c)] -- 12.1 Expansion about the critical temperature -- 12.1.1 Functional Taylor expansions -- 12.1.2 Diagrammatic representation of the Φ[sup(2)] correlation functions -- 12.1.3 Wavevector space -- 12.1.4 Vertex functions -- 12.1.5 Renormalization -- 12.1.6 Expanding the renormalized vertex functions. , 12.1.7 The validity of the expansion -- 12.2 The renormalization group equations -- 12.2.1 The exponent v -- 12.2.2 The exponent γ -- 12.2.3 The exponent α -- 12.3 The renormalization group below T[sub(c)] -- 12.3.1 The exponent β -- 12.4 Calculating γ[sub(2)] to one loop -- Problems -- 13 The lower critical dimension -- 13.1 Order below T[sub(c)] -- 13.1.1 The case D = 1 -- 13.1.2 Systems with more than one component -- 13.1.3 Goldstone modes -- 13.2 The non-linear σ-model -- 13.2.1 The two-point vertex function -- 13.2.2 The renormalization group equation -- 13.3 The Kosterlitz-Thouless transition -- 13.3.1 The two-dimensional Coulomb gas -- 13.3.2 General Remarks -- Problems -- 14 Universality -- 14.1 Perturbing the Gaussian Hamiltonian -- 14.1.1 The applicability of these results -- 14.2 Perturbing the Landau-Ginzburg Hamiltonian -- 14.2.1 The case of three dimensions -- 14.2.2 The case of two dimensions -- 14.3 Relevance and renormalizability -- Problems -- Appendices -- A: The magnetic scattering of neutrons -- B: The natural variables for thermodynamic potentials -- C: Magnetic energy -- D: Connected correlation functions and log Z[J] -- E: The Gibbs free energy -- F: Discrete Fourier transforms -- G: The method of steepest descent -- H: Counting closed loops on a square lattice -- I: Einstein's fluctuation theory -- J: The Gaussian transformation -- K: The Landau-Ginzburg model and the Ising model -- L: Functional differentiation and integration -- M: The Feynman rules for the vertex functions -- N: Feynman rules for generalized Landau-Ginzburg models -- Answers -- References -- Index -- A -- B -- C -- D -- E -- F -- G -- H -- I -- J -- K -- L -- M -- N -- O -- P -- Q -- R -- S -- T -- U -- V -- W -- X -- Z.
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  • 2
    Electronic Resource
    Electronic Resource
    Palo Alto, Calif. : Annual Reviews
    Annual Review of Astronomy and Astrophysics 30 (1992), S. 51-74 
    ISSN: 0066-4146
    Source: Annual Reviews Electronic Back Volume Collection 1932-2001ff
    Topics: Physics
    Type of Medium: Electronic Resource
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  • 3
    Electronic Resource
    Electronic Resource
    [s.l.] : Macmillan Magazines Ltd.
    Nature 392 (1998), S. 471-473 
    ISSN: 1476-4687
    Source: Nature Archives 1869 - 2009
    Topics: Biology , Chemistry and Pharmacology , Medicine , Natural Sciences in General , Physics
    Notes: [Auszug] It is now over 40 years since radio observations of neutral hydrogen revealed the gaseous disk of our Galaxy to be warped. Subsequently, the warp has been detected in the distribution of Galactic dust, molecular clouds, and luminous stars,. Roughly half of all spiral galaxies have similarly ...
    Type of Medium: Electronic Resource
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  • 4
    Electronic Resource
    Electronic Resource
    [s.l.] : Nature Publishing Group
    Nature 365 (1993), S. 20-20 
    ISSN: 1476-4687
    Source: Nature Archives 1869 - 2009
    Topics: Biology , Chemistry and Pharmacology , Medicine , Natural Sciences in General , Physics
    Notes: [Auszug] SIR - Battaner et al.1 argue that the flat rotation curves of galaxies such as M31 may be caused not by dark matter, but by magnetic tension. In essence they suggest that the centripetal force required to hold together a rapidly spinning disk of gas is-provided by the tension of an azimuthal ...
    Type of Medium: Electronic Resource
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  • 5
    Publication Date: 2013-07-04
    Description: We consider the problem of determining the Galaxy's gravitational potential from a star catalogue. We show that orbit-based approaches to this problem suffer from unacceptable numerical noise deriving from the use of only a finite number of orbits. An alternative approach, which requires an ability to determine the model's phase-space density at predetermined positions and velocities, has a level of numerical noise that lies well below the intrinsic uncertainty associated with the finite size of the catalogue analysed. A catalogue of 10 000 stars brighter than V  = 17 and distributed over the sky at b  〉 30° enables us to determine the scaleheight of the disc that contributes to the potential with an uncertainty below 20 pc if the catalogue gives proper motions, line-of-sight velocities and parallaxes with errors typical of the Gaia Catalogue, rising to 36 pc if only proper motions are available. The uncertainty in the disc's scalelength is significantly smaller than 0.25 kpc.
    Print ISSN: 0035-8711
    Electronic ISSN: 1365-2966
    Topics: Physics
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