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Über dieses Buch

Stable Isotope Geochemistry is an introduction to the use of stable isotopes in the geosciences. It is subdivided into three parts:

- theoretical and experimental principles;

- fractionation mechanisms of light and heavy elements;

- the natural variations of geologically important reservoirs.

The 5th edition has been revised and extended and now includes a new chapter on palaeoclimatology. Special emphasis has been given to the growing field of "heavy" elements. Many new references have been added, which will enable quick access to recent literature. For students and scientists alike the book will be a primary source of information with regard to how and where stable isotopes can be used to solve geological problems.



Chapter 1. Theoretical and Experimental Principles

Isotopes are atoms whose nuclei contain the same number of protons but a different number of neutrons. The term “isotope” is derived from Greek (meaning equal places) and indicates that isotopes occupy the same position in the periodic table.
Jochen Hoefs

Chapter 2. Isotope Fractionation Mechanisms of Selected Elements

The foundations of stable isotope geochemistry were laid in 1947 by Urey’s classic paper on the thermodynamic properties of isotopic substances and by Nier’s development of the ratio mass spectrometer. Before discussing details of the naturally occurring variations in stable isotope ratios, it is useful to describe some generalities that are pertinent to the field of nonradiogenic isotope geochemistry as a whole.
Jochen Hoefs

Chapter 3. Variations of Stable Isotope Ratios in Nature

Isotope variations found in extraterrestrial materials have been classified according to different processes — such as chemical mass fractionation, nuclear reactions, nucleosynthesis — and/or to different sources — such as interplanetary dust, solar materials, and comet material. Various geochemical fingerprints point to the reservoir from which the planetary sample was derived and the environment in which the sample has formed. They can be attributed to a variety of processes, ranging from heterogeneities in the early solar nebula to the evolution of a planetary body. For more details, the reader is referred to reviews of Thiemens (1988), Clayton (1993), and McKeegan and Leshin (2001).
Jochen Hoefs


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