The Evolution of Matter: From the Big Bang to the Present Day
Language: English
Pages: 532
ISBN: 052116964X
Format: PDF / Kindle (mobi) / ePub
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 geochemistry, this volume follows the chemical history of matter from the very beginning to the present, demonstrating connections in space and time. It provides also solid links from cosmochemistry to the geochemistry of Earth. The book presents comprehensive descriptions of the various isotope systematics and fractionation processes occurring naturally in the Universe, using simple equations and helpful tables of data. With a glossary of terms and over 900 references, this volume is a valuable reference for researchers and advanced students studying the chemical evolution of the Earth, the Solar System and the wider Universe.
Absolutely Small: How Quantum Theory Explains Our Everyday World
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Quo Vadis Quantum Mechanics? (The Frontiers Collection)
Understanding the Universe: From Quarks to the Cosmos
very metal-deficient stars show that the abundance ratios of light and heavy n-capture elements, e.g. Sr/Ba, scatter over more than an order of magnitude even though both are mainly generated in s-process nucleosynthesis. This implies the production of the lighter elements in different nucleosynthetic processes. Beers and Christlieb (2005) presented a detailed review of this new and exciting topic of astrophysics. 3.3 Presolar grains Dust is an important host for the heavy refractory elements in
elements and some proton-rich nuclides during star explosions (Wilson et al., 1986; Woosley et al., 1990). The flux of neutrinos through the expanding envelope is so great that despite the small cross sections significant nuclear transmutations become possible. Neutrinos excite heavy nuclei to particleunbound levels: the expulsion of a single neutron, proton or α-particle yields a new element: (Z , A) + ν → (Z , A)∗ + ν → (Z , A − 1) + n + ν ; → (Z − 1, A − 1) + p + ν ; → (Z − 2, A − 4) + α + ν .
stars. Trace s-process elements are underabundant at low metallicities; their abundance, along with the [s-process/r-process] value, increases smoothly with time. This is explained by the generation of s-process elements in low-mass stars, which live longer than massive stars. Grains in the interstellar medium have preserved a high-resolution record of the evolution of stable isotopes as well as vestiges of the decay of short-lived nuclides. The stable isotopes provide constraints for models of
Reservoir Table 11.4 Isotopic compositions of Xe in several important reservoirs (100 × i Xe/130 Xe)a 11 Chondritic meteorites 151 oxidants, such as HNO3 , while it is resistant when non-oxidizing solvents are used (HF or HCl; Wieler et al., 1991). (2) The extraction patterns for carbon and heavy primordial gases in combustion experiments are similar (Ott et al., 1984). (3) The carbon-rich low-density phase of a meteorite contains more than 99% of the “Q” component (Frick and Chang, 1978;
99.4 Nuevo Laredo Nuevo Laredo trend Eucrites (main group) 50.3 0.30 8.30 0.69 17.5 0.50 15.8 5.20 0.28 0.02 n.d. n.d. 98. 9 Kapoeta 50.8 0.23 4.27 1.02 16.7 0.52 21.4 3.83 0.13 0.01 n.d. 0.11 99.0 Y-7308 Howardites Table 12.1 Major-element compositions (wt %) of diogenites, eucrites and howardites. From Mittlefehldt et al. (1998). Reproduced by permission of the Mineralogical Society of America b 9.9 n.d. 18 n.d. n.d. n.d. 0.009 n.d. 0.004 0.002 n.d. n.d. n.d. n.d. 0.03 0.006 n.d.
