An Introduction to Modern CosmologyAn Introduction to Modern Cosmology Third Edition is an accessible account of modern cosmological ideas. The Big Bang Cosmology is explored, looking at its observational successes in explaining the expansion of the Universe, the existence and properties of the cosmic microwave background, and the origin of light elements in the universe. Properties of the very early Universe are also covered, including the motivation for a rapid period of expansion known as cosmological inflation. The third edition brings this established undergraduate textbook up-to-date with the rapidly evolving observational situation. This fully revised edition of a bestseller takes an approach which is grounded in physics with a logical flow of chapters leading the reader from basic ideas of the expansion described by the Friedman equations to some of the more advanced ideas about the early universe. It also incorporates up-to-date results from the Planck mission, which imaged the anisotropies of the Cosmic Microwave Background radiation over the whole sky. The Advanced Topic sections present subjects with more detailed mathematical approaches to give greater depth to discussions. Student problems with hints for solving them and numerical answers are embedded in the chapters to facilitate the reader’s understanding and learning. Cosmology is now part of the core in many degree programs. This current, clear and concise introductory text is relevant to a wide range of astronomy programs worldwide and is essential reading for undergraduates and Masters students, as well as anyone starting research in cosmology. |
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Page 39
... number densities An important alternative view of the evolution of particles , which will be much used later in the book , is that of the number density n of particles rather than of their mass or energy density . The number density is ...
... number densities An important alternative view of the evolution of particles , which will be much used later in the book , is that of the number density n of particles rather than of their mass or energy density . The number density is ...
Page 77
... number density of photons , while the redshifting reduces their frequency . In combination , these two effects map ... number densities simply reduce in inverse proportion to the volume , n x 1 / a3 . This is true of both protons and ...
... number density of photons , while the redshifting reduces their frequency . In combination , these two effects map ... number densities simply reduce in inverse proportion to the volume , n x 1 / a3 . This is true of both protons and ...
Page 92
... number density N is given by mc2 Ναm3 / 2 exp kBT :) . ( 12.1 ) [ I'm using N for number density in this section to avoid confusion with ' n ' for neutron ; N is the same as the number density n of Section 5.4 and elsewhere . ] The ...
... number density N is given by mc2 Ναm3 / 2 exp kBT :) . ( 12.1 ) [ I'm using N for number density in this section to avoid confusion with ' n ' for neutron ; N is the same as the number density n of Section 5.4 and elsewhere . ] The ...
Contents
Constants conversion factors and symbols | 1 |
Eales Coel Hellier and Linda Smith for numerous detailed comments which led to | 3 |
What particles are there? | 11 |
Copyright | |
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abundances acceleration equation Advanced Topic angular diameter distance anisotropies assuming atoms baryon number baryonic matter black-body Chapter coordinates corresponding cosmic microwave background cosmological constant cosmological models cosmological principle cosmologists critical density curvature curves dark matter decay deceleration deceleration parameter decoupling density parameter derivation discussed distribution electrons energy density epoch estimate evolution expansion rate flat geometry fluid equation Friedmann equation galaxy clusters given gives helium-4 Hot Big Bang Hubble constant Hubble parameter inflation inflationary interactions ionization known luminosity distance mass mass-energy material matter density matter dominated means measured megaparsecs metric non-relativistic nuclei nucleosynthesis number density observable Universe particle physics photons possible predicted present Universe Problem properties protons and neutrons radiation dominated radius redshift region relative relativistic scale factor shown in Figure solution space-time spatially-flat spectrum sphere spherical stars structure formation supernovae surface temperature theory thermal equilibrium topology typical Universe expands velocity Ωο