Download e-book for kindle: Planetary Crusts : Their Composition, Origin and Evolution by S. Ross Taylor, Scott McLennan

By S. Ross Taylor, Scott McLennan

ISBN-10: 0511463820

ISBN-13: 9780511463822

ISBN-10: 0521841860

ISBN-13: 9780521841863

This reference quantity offers an updated survey of the improvement of crusts on strong planets and satellites within the sunlight System.

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12. 88 × 1010 years. 13. The causes of this depletion are much debated. Initial suggestions that the depletion was due to condensation or evaporation in a hot nebula have been ruled out by the absence of Notes and references 14. 15. 16. 17. 18. 19. g. in K) and the astrophysical evidence that nebular disks are cool (a few hundred Kelvin). So the nebula was cool, not hot and the notion of elements condensing from a hot nebula is no longer tenable. Observations of midplane temperatures in disks around T Tauri stars give values mostly less than 600 K at 1 AU (Valenti, J.

94 246 928 712 134 560 Ref. 1 * Two estimates of the composition of type CI carbonaceous chondrites. (1) Mean CI abundances from Palme, H. and Jones, A. (2004) in Treatise on Geochemistry (eds. H. D. Holland and K. K. Turekian), Elsevier, vol. 03, Table 3, p. 49. (2) Mean CI chondrite composition from Anders, E. and Grevesse, N. (1989) GCA 53, Table 1, p. 158. Little significant change has occurred in the 15 year interval between the two estimates. 10 1 The planets: their formation and differentiation respectively, contain only 1 or 2 Earth-masses of gas and are mostly composed of ice and rock.

18. 19. g. in K) and the astrophysical evidence that nebular disks are cool (a few hundred Kelvin). So the nebula was cool, not hot and the notion of elements condensing from a hot nebula is no longer tenable. Observations of midplane temperatures in disks around T Tauri stars give values mostly less than 600 K at 1 AU (Valenti, J. A. (1993) T Tauri stars in blue. Astron. J. 106, 2024–50; Hartmann, L. (1998) Accretion and evolution of T Tauri stars. Astrophys. J. 495, 385–400). However close to the Sun, refractory inclusions that constitute a few percent of meteorites were formed in the X-wind environment at high temperatures (Shu, F.

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Planetary Crusts : Their Composition, Origin and Evolution by S. Ross Taylor, Scott McLennan


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