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1. An introduction to modern cosmology [2015]
 Liddle, Andrew R., author.
 Third edition.  Chichester, West Sussex : John Wiley and Sons, Inc., 2015.
 Description
 Book — xv, 182 pages : illustrations ; 23 cm
 Summary

 Preface xi Constants, conversion factors and symbols xiv
 1 A (Very) Brief History of Cosmological Ideas
 1
 2 Observational Overview
 3 2.1 In visible light
 3 2.2 In other wavebands
 6 2.3 Homogeneity and isotropy
 10 2.4 The expansion of the Universe
 10 2.5 Particles in the Universe
 13
 3 Newtonian Gravity
 21 3.1 The Friedmann equation
 22 3.2 On the meaning of the expansion
 25 3.3 Things that go faster than light
 25 3.4 The fluid equation
 26 3.5 The acceleration equation
 27 3.6 On mass, energy and vanishing factors of c2
 28
 4 The Geometry of the Universe
 29 4.1 Flat geometry
 29 4.2 Spherical geometry
 30 4.3 Hyperbolic geometry
 32 4.4 Infinite and observable Universes
 33 4.5 Where did the Big Bang happen?
 33 4.6 Three values of k
 34
 5 Simple Cosmological Models
 37 5.1 Hubble s law
 37 5.2 Expansion and redshift
 38 5.3 Solving the equations
 39 5.4 Particle number densities
 43 5.5 Evolution including curvature
 44
 6 Observational Parameters
 49 6.1 The expansion rate H0
 49 6.2 The density parameter
 0
 51 6.3 The deceleration parameter q0
 52
 7 The Cosmological Constant
 55 7.1 Introducing 
 55 7.2 Fluid description of 
 56 7.3 Cosmological models with 
 57
 8 The Age of the Universe
 61
 9 The Density of the Universe and Dark Matter
 67 9.1 Weighing the Universe
 67 9.2 What might the dark matter be?
 73 9.3 Dark matter searches
 74
 10 The Cosmic Microwave Background
 77 10.1 Properties of the microwave background
 77 10.2 The photon to baryon ratio
 79 10.3 The origin of the microwave background
 80 10.4 The origin of the microwave background (advanced)
 83
 11 The Early Universe
 87
 12 Nucleosynthesis: The Origin of the Light Elements
 93 12.1 Hydrogen and Helium
 93 12.2 Comparing with observations
 96 12.3 Contrasting decoupling and nucleosynthesis
 98
 13 The Inflationary Universe
 101 13.1 Problems with the Hot Big Bang
 101 13.2 Inflationary expansion
 105 13.3 Solving the Big Bang problems
 106 13.4 How much inflation?
 108 13.5 Inflation and particle physics
 109
 14 The Initial Singularity
 113
 15 Overview: The Standard Cosmological Model
 117 Advanced Topic
 1 General Relativistic Cosmology
 121 1.1 The metric of spacetime
 121 1.2 The Einstein equations
 122 1.3 Aside: Topology of the Universe
 124 Advanced Topic
 2 Classic Cosmology: Distances and Luminosities
 127 2.1 Light propagation and redshift
 127 2.2 The observable Universe
 130 2.3 Luminosity distance
 130 2.4 Angular diameter distance
 134 2.5 Source counts
 136 Advanced Topic
 3 Neutrino Cosmology
 139 3.1 The massless case
 139 3.2 Massive neutrinos
 141 3.3 Neutrinos and structure formation
 142 Advanced Topic
 4 Baryogenesis
 145 Advanced Topic
 5 Structures in the Universe
 149 5.1 The observed structures
 149 5.2 Gravitational instability
 151 5.3 The clustering of galaxies
 152 5.4 Cosmic microwave background anisotropies
 154 5.5 The origin of structure
 159 Advanced Topic
 6 Constraining cosmological models
 163 6.1 Cosmological models and parameters
 163 6.2 Key cosmological observations
 164 6.3 Cosmological data analysis
 164 6.4 The Standard Cosmological Model:
 2014 edition
 166 6.5 The future
 168 Bibliography
 171 Numerical answers and hints to problems
 173 Index 177.
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QB981 .L534 2015  Unknown 
2. The Oxford companion to cosmology [2008]
 Liddle, Andrew R.
 Oxford ; New York : Oxford University Press, 2008.
 Description
 Book — xv, 343 p. : ill. ; 24 cm.
 Summary

 PREFACE GLOSSARY COMMONLY USED SYMBOLS OVERVIEW: THE HOT BIG BANG COSMOLOGY THE OXFORD COMPANION TO COSMOLOGY AZ INDEX.
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QB981 .L535 2008  Inlibrary use 
 Liddle, Andrew R.
 [Oxford] : Oxford University Press, 2008
 Description
 1 online resource.
 Database topics
 Uncategorized
 Summary

This companion includes over 350 entries, extensively crossreferenced, describing the modern view of cosmology including both theoretical ideas and the many strands of observational evidence.
 Liddle, Andrew R.
 Cambridge ; New York : Cambridge University Press, 2000.
 Description
 Book — xiii, 400 p. : ill. ; 25 cm.
 Summary

 1. Introduction
 2. The hot Big Bang cosmology
 3. Inflation
 4. The simplest model for the origin of structure I
 5. The simplest model for the origin of structure II
 6. Extensions to the smplest model
 7. Scalar fields and the vacuum fluctuation
 8. Building and testing models of inflation
 9. The cosmic microwave background
 10. Galaxy motions and clustering
 11. The QuasiLinear regime
 12. Putting observations together
 13. Outlook for the future
 14. Advanced topic: cosmological Perturbation theory
 15. Advanced topic: diffusion and free streaming Index.
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QB991 .I54 L53 2000  Unknown 
5. An introduction to modern cosmology [1999]
 Liddle, Andrew R.
 Chichester ; New York : Wiley, c1999.
 Description
 Book — xiii, 129 p., 4 p. of plates : ill. (some col.) ; 25 cm.
 Summary

 History of Cosmological Ideas. Observational Overview. Newtonian Gravity. Newtonian Cosmological Models. Geometry of the Universe. Observational Parameters. Age of the Universe. Density of the Universe and Dark Matters. Microwave Background. The Early Universe. Origin of Light Elements. Inflationary Universe Theory. Initial Singularity. Appendix. Index.
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This new textbook provides a readable and accessible introduction to the subject for those students taking a first course in cosmology. An Introduction to Modern Cosmology introduces models of the expanding universe and explores all the successes of the hot big bang, including the cosmic microwave background and nucleosynthesis. A brief discussion of the inflationary cosmology is also included. No prior knowledge of astronomy is assumed and the book's general approach tends to avoid relativity, deriving the crucial results using newtonian theory. This allows a discussion of all the evidence in favour of the hot big bang in a treatment which is based in physics rather than mathematics.
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QB981 .L534 1999  Available 
 Liddle, Andrew R.
 Batavia, IL : Fermi National Accelerator Laboratory ; [Washington, DC : National Aeronautics and Space Administration ; Springfield, Va. : National Technical Information Service, distributor, 1994?]
 Description
 Book — 1 v.
 Online
Green Library
Green Library  Status 

Find it US Federal Documents  
NAS 1.26:197629  Unknown 
 Lyth, D. H. (David Hilary)
 Cambridge, UK ; New York : Cambridge University Press, 2009.
 Description
 Book — xviii, 497 p. : ill. ; 26 cm.
 Summary

 1. Overview Part I. Relativity:
 2. Special relativity
 3. General relativity Part II. The Universe after the First Second:
 4. The unperturbed Universe
 5. The primordial density perturbation
 6. Stochastic properties
 7. Newtonian perturbations
 8. General relativistic perturbations
 9. The matter distribution
 10. Cosmic microwave background anistropy
 11. Boltzmann hierarchy and polarization
 12. Isocurvature and tensor modes Part III. Field Theory:
 13. Scalar fields and gravity
 14. Internal symmetry
 15. Quantum field theory
 16. The Standard Model
 17. Supersymmetry Part IV. Inflation and the Early Universe:
 18. Slowroll inflation
 19. More inflation paradigms
 20. Reheating and phase transitions
 21. Baryon number, CDM and dark energy
 22. Generating field perturbations at horizon exit
 23. Generating zeta at horizon exit
 24. Generating zeta and Si after horizon exit
 25. Slowroll inflation and observation Appendixes Index.
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Engineering Library (Terman)
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QB361 .L98 2009  Unknown 
 Copeland, Edmund J.
 [Batavia, Ill.] : Fermi National Accelerator Laboratory, [1990]
 Description
 Book — 1 v.
Green Library
Green Library  Status 

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NAS 1.26:186594  Unknown 
 Washington, D.C. : United States. Dept. of Energy. High Energy Physics Division ; Oak Ridge, Tenn. : distributed by the Office of Scientific and Technical Information, U.S. Dept. of Energy, 1994
 Description
 Book — 1 online resource (13 pages ) : digital, PDF file.
 Summary

Abstract Not Provided
 Online
 Washington, D.C. : United States. Dept. of Energy. High Energy Physics Division ; Oak Ridge, Tenn. : distributed by the Office of Scientific and Technical Information, U.S. Dept. of Energy, 1994
 Description
 Book — 1 online resource (18 pages ) : digital, PDF file.
 Summary

We use numerical simulations to calculate the cosmic microwave background anisotropy induced by the evolution of a global texture field, with special emphasis on individual textures. Both spherically symmetric and general configurations are analyzed, and in the latter case we consider field configurations which exhibit unwinding events and also ones which do not. We compare the results given by evolving the field numerically under both the expanded core (XCORE) and nonlinear sigma model (NLSM) approximations with the analytic predictions of the NLSM exact solution for a spherically symmetric selfsimilar (SSSS) unwinding. We find that the random unwinding configuration spots' typical peak height is 6075\% and angular size typically only 10% of those of the SSSS unwinding, and that random configurations without an unwinding event nonetheless may generate indistinguishable hot and cold spots. A brief comparison is made with other work.
 Online
 Washington, D.C. : United States. Dept. of Energy. High Energy Physics Division ; Oak Ridge, Tenn. : distributed by the Office of Scientific and Technical Information, U.S. Dept. of Energy, 1993
 Description
 Book — 1 online resource (9 pages ) : digital, PDF file.
 Summary

One method to reconstruct the scalar field potential of inflation is a perturbative approach, where the values of the potential and its derivatives are calculated as an expansion in departures from the slowroll approximation. They can then be expressed in terms of observable quantities, such as the square of the ratio of the gravitational wave amplitude to the density perturbation amplitude, the deviation of the spectral index from the HarrisonZel'dovich value, etc. Here, we calculate complete expressions for the secondorder contributions to the coefficients of the expansion by including for the first time corrections to the standard expressions for the perturbation spectra. As well as offering an improved result, these corrections indicate the expected accuracy of the reconstruction. Typically the corrections are only a few percent.
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