Structure formation in the universe / T. Padmanabhan.

Format:

• Book

Author/Creator:

• Padmanabhan, T. (Thanu), 1957-2021.

Language:

English

Subjects (All):

• Cosmology.
• Astrophysics.

Physical Description:

xvi, 483 pages : illustrations ; 25 cm

Place of Publication:

Cambridge ; New York : Cambridge University Press, 1993.

Summary:

• Understanding the way in which large-scale structures like galaxies form remains the most challenging problem in cosmology today. This text provides an up-to-date and pedagogical introduction to this exciting area of research. Part 1 deals with the Friedmann model, the thermal history of the universe, and includes a description of observed structures in the universe. Part 2 describes the theory of gravitational instability in the linear regime, and the statistics of density fields. This part also includes chapters on the microwave background radiation and large scale velocity fields. Part 3 of the book covers nonlinear instability, high redshift objects, inflation, cosmic strings and dark matter. Each chapter is accompanied by a comprehensive set of exercises to help the reader in self-study.
• The book will be of interest to research and graduate students in cosmology, relativity, theoretical physics, astrophysics and astronomy. It is also suitable for use as a graduate textbook for introductory graduate level courses.
• The diagram on the cover shows the distribution of galaxies in the universe around us. It is derived from a density plot out to 325 million light years using the QDOT (QMW -- Durham -- Oxford -- Toronto) all-sky redshift survey of galaxies detected by the IRAS satellite. The Local Supercluster (including our own Milky Way) lies near the centre of the plot with A1367, Coma, A2197/2199 and Hercules joining together to form part of the Great Wall in the Northern Hemisphere, with Hercules along the top right limb. Joined to this huge structure with a bridge of galaxies passing through the galactic plane are Perseus -- Pisces and N1600. Other newly detected superclusters(S3, S6) are shown at the foot of the diagram, below the Perseus -- Pisces trunk. The Pavo -- Indus structure seems to be floating to the immediate right of the lower trunk. Shapley's supercluster is floating immediately above it with the Hydra -- Centaurus cluster extending from the main body behind it. The high level of connectedness in the distribution is symptomatic of a 'sponge-like' topology and provides information on the nature of primordial density fluctuations produced in the Big Bang.

Contents:

• Part 1 The smooth universe 1
• 1 Introducing the universe 3
• 1.2 Existence of large scale structures 3
• 1.3 Stars 8
• 1.4 Galaxies 15
• 1.5 Models for galaxies 20
• 1.6 Distribution of matter 25
• 1.7 Expansion of the universe 28
• 1.8 Quasars 31
• 1.9 Radiation in the universe 34
• 1.10 Determination of extragalactic distances 37
• 1.11 Age of various structures 40
• 2 The Friedmann model 49
• 2.2 The Friedmann model 49
• 2.3 Kinematic properties of the Friedmann universe 54
• 2.4 Dynamics of the Friedmann model 59
• 2.5 Radiative processes in the expanding universe 70
• 2.6 The Hubble radius 73
• 3 Thermal history of the universe 82
• 3.2 Distribution functions in the early universe 82
• 3.3 Relic background of relativistic particles 90
• 3.4 Relic background of wimps 96
• 3.5 Synthesis of light nuclei 101
• 3.6 Decoupling of matter and radiation 108
• Part 2 The clumpy universe 123
• 4 Linear theory of perturbations 125
• 4.2 Suppression and growth of inhomogeneities 125
• 4.3 The linear perturbation theory 136
• 4.4 Gravitational instability in the relativistic case 149
• 4.5 Solutions to the Newtonian perturbation equation 160
• 4.6 Dissipation in dark matter and baryons 167
• 4.7 The processed final spectrum 173
• 5 Statistical properties 186
• 5.2 Probability functionals 186
• 5.3 Gaussian probability functional 189
• 5.4 Spatial averages and filter functions 194
• 5.5 Normalization of the fluctuation spectrum 200
• 5.6 The time evolution of the correlation function 203
• 5.7 Correlation of high density regions 206
• 5.8 Mass functions 210
• 6 Microwave background radiation 217
• 6.2 Processes leading to distortions in the MBR 217
• 6.3 Propagation of light in a perturbed universe 222
• 6.4 Anisotropy due to variations in the potential 228
• 6.5 Anisotropies due to peculiar velocities 231
• 6.6 Intrinsic anisotropies 233
• 6.7 Damping of the anisotropies 237
• 6.8 Spectral distortions due to the ionized gas 239
• 7 Velocity fields 248
• 7.2 Large scale velocity fields 248
• 7.3 Theoretical constraints on peculiar velocities 261
• Part 3 Towards a more complete picture 271
• 8 The nonlinear evolution 273
• 8.2 Spherical model for the nonlinear collapse 273
• 8.3 Scaling laws 285
• 8.4 The masses of galaxies 287
• 8.5 Zeldovich approximation 294
• 8.6 The adhesion model 299
• 8.7 The angular momentum of galaxies 305
• 8.8 Formation of disc galaxies 307
• 8.9 Formation of elliptical galaxies 310
• 8.10 Nonlinear evolution using N-body simulations 313
• 9 High redshift objects 325
• 9.2 Primeval galaxies 325
• 9.3 Quasars and galaxy formation 331
• 9.4 Absorption spectra of quasars 339
• 9.5 High redshift radio galaxies 349
• 10 The origin of perturbations 353
• 10.2 The concept of inflation 353
• 10.3 The epicycles of inflation 360
• 10.4 Origin of density perturbations 364
• 10.5 Cosmic strings 373
• 11 Dark matter 382
• 11.2 Observational evidence for dark matter 382
• 11.3 Nature of dark matter 395
• 11.4 Massive neutrinos 401
• 11.5 Axions 404
• 11.6 Cosmological constant as dark matter 407
• 12 Epilogue 415
• 12.2 Structure formation - an appraisal 415
• Appendix A Aspects of general relativity 423
• Appendix B Aspects of field theory 439
• Appendix C COBE results and implications 445
• Some useful numbers 474.

Notes:

Includes bibliographical references (pages 451-473) and index.

ISBN:

• 0521414482
• 0521424860

OCLC:

25711383