Evolution solar system

S. R. Taylor, Solar System Evolution, Cambridge University Press, Cambridge, UK, 1992. 

The geological sciences are involved in studying the naturally occurring materials of the earth and solar system (i) to understand the fimdamental processes of crustal formation on earth and solar system evolution, and (2) to evaluate the crustal materials of potential economic value to man. Prior to the 1930 s, analyses were carried out exclusively using classical analytical techniques, with detection limits on the order of o.oi-o.i % (mass fraction). The number of elements contained in any sample could be as extensive as the periodic table, but very few of these could be determined. The development of instrumental techniques revolutionized the analysis of geochemical samples, beginning in the 1930 s. 

Marhas, . ., Goswami, J.N. and Davis, A. M. (2002) Short-lived nuclides in hibonite grains from Murchison evidence for solar system evolution. Science, 298, 2182-2185. 

Taylor, S. R. (1992) Solar System Evolution A New Perspective. Cambridge Cambridge University Press, 307 pp. A thorough treatise that covers ideas about the origin and evolution of the terrestrial planets. 

So the ability to measure W isotopic compositions with MC-ICP-MS has immediately opened up exciting new scientific opportunities of broad significance. In a similar manner the technique could be used to develop other chronometers of early solar system evolution, previously intractable. 

Chondritic meteorites contain a complex record of processes that occurred during the earliest stages of solar system evolution, from the formation of the earliest solids by condensation in the solar nebula to the accretion of asteroidal... 

Chondritic Meteorites as Probes of Early Solar System Evolution... 

Meteorites are extremely important to our understanding of solar system evolution, because, in their most primitive form, they are our most ancient samples of the solar system. As such they provide valuable information about the condensation of the solar nebula from which our solar system formed. Whilst they represent, to date, our most abundant sample of extraterrestrial material, we have no... 

LONG-LIVED NUCLIDES CHRONOLOGY OF SOLAR SYSTEM EVOLUTION... 

Taylor S, Herzog GF, Delaney JS (2007) Crumbs from the crust of Vesta Achondritic cosmic spherules from the South Pole water well. Meteorit Planet Sci 42(2) 223-233 Taylor SR (1992) Solar system evolution a new perspective. 

REE patterns in bulk carbonaceous chondrites are fairly uniform, parallel to Cl, and show no dependence on volatility (e.g., no Eu or Yb anomalies). This uniformity also applies to the ordinary (H, E, EE classes) and enstatite (EL, EH classes) chondrite classes that show significant loss of their moderately and highly volatile elements (e.g., potassium, lead) and/or variations in their metal/silicate ratios. Accordingly, REE abundances in chondritic meteorites indicate no substantial cosmochemical fractionation (i.e., volatile related redox related) during their formation in the early stages of solar system evolution and indicate broad homogeneity in the solar nebula. 

The ratio of the total emitted power to the absorbed power is customarily called the energy balance of a planet. First, we consider the determination of this quantity for the Earth and by implication for the other terrestrial bodies. Then we review measurements of the energy balance of the outer planets. In that process we discuss the implications of the internal heat sources for theories of Solar System evolution. 

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