The Evolution of Matter : From the Big Bang to the Present Day

The Evolution of Matter : From the Big Bang to the Present Day / Igor Tolstikhin, Jan Kramers.

The Evolution of Matter explains how all matter in the Universe developed following the Big Bang and through subsequent stellar processes. It describes the evolution of interstellar matter and its differentiation during the accretion of the planets and the history of the Earth. Unlike many books on...

Full description

Saved in:
Bibliographic Details
Corporate Author: Cambridge University Press
Other Authors: Tolstikhin, Igor, Kramers, Jan
Format: eBook
Language:English
Published: Cambridge : Cambridge University Press, 2008.
Subjects:
Isotope geology.
Interstellar matter.
Molecular evolution.
Matter.
Cosmology.
cosmology.
Cosmology
Interstellar matter
Isotope geology
Matter
Molecular evolution
Online Access:Click for online access
Table of Contents:
  • Cover; Half-title; Title; Copyright; Contents; Introduction; Part I: The elements ; 1 Isotopes: weights and abundances; 1.1 Introduction: nuclei and their behaviour; 1.2 Atomic nuclei and binding energy, with some predictions on isotope abundances; Mass, energy and binding energy; Relationships between binding energy and atomic mass; Odd, even and even-odd families; Heavy elements and radioactive isotopes; 1.3 Summary; 2 Introduction to the Universe: the baryonic matter; 3 Element and isotope abundances: reference collection; 3.1 Hydrogen and helium and their special significance.
  • 3.2 Metal-poor stars: the most ancient matter of the Galaxy3.3 Presolar grains; 3.4 The solar system element and isotope abundances; Environments, processes and behaviour of the elements: some phenomenology; C1-meteorite, solar and terrestrial element and isotope abundances: a comparison; Solar system elemental and isotope abundances; Solar system sample of short-lived nuclides; 3.5 Summary; 4 Cosmological nucleosynthesis: production of H and He; 4.1 The expanding Universe and the Big Bang hypothesis; 4.2 Big Bang nucleosynthesis (BBN); 4.3 The age of the Universe.
  • Distance-redshift relationship: Doppler effect and redshiftDistance-redshift relationship: distances; The Hubble parameter and the age of the Universe; 4.4 Summary; 5 Stellar nucleosynthesis: lower-mass stars and the s-process; 5.1 Introduction; 5.2 Formation of stars; 5.3 Hydrogen and He burning and the evolution of a low-mass star; Hydrogen burning; Helium burning; 5.4 Slow nucleosynthesis (s-process); What is meant by ""slow""?; Neutron sources; S-process and non-s-process species; Comparison of model-derived and observed s-process nuclide abundances.
  • Stellar B-decay enhancement: are the decay constants really constant and are the stable isotopes really stable?Branching: isotope abundance as a measure of neutron density in the s-process environment; 5.5 Summary; 6 Stellar nucleosynthesis: r- and associated processes; 6.1 Introduction to rapid nucleosynthesis (r-process): what does ""rapid"" mean?; 6.2 Evolution of massive stars; 6.3 Core-collapse supernovae (SNe II) and rapid nucleosynthesis Supernovae type II (SNe II) ; Explosive nucleosynthesis: r-process and explosive burning; Associated p-, y- and v- process.
  • Special significance of 56 Ni and 44 Ti: bright isotopic candles 6.4 SNe Ia: nucleosynthesis and luminosity; 6.5 Summary; 7 Timing of stellar nucleosynthesis; 7.1 Cosmochronology from long-lived radioactive elements; 7.2 The uranium isotopes: age and evolution of stellar nucleosynthesis; 7.3 The age of stellar clusters: luminosity temperature relationships; 7.4 Summary; 8 Chemical evolution of the Galaxy; 8.1 Introduction: processes governing galactic chemical evolution; 8.2 Milky Way evolution; The [Fe/H]-age reference evolution; The CNO elements.

Similar Items