Terrestrial planets evolution

Candela, P. A. (1986). Generalized mathematical models for the fractional evolution of vapor from magmas in terrestrial planetary crusts. In Chemistry and Physics of Terrestrial Planets, ed. E. K. Saxena, pp. 362-96. NY Springer. 

Kleine, T., Touboul, M., Bourdon, B. et al. (2009) Hf-W chronology of the accretion and early evolution of asteroids and terrestrial planets. Geochimica et Cosmochimica Acta,... 

Pepin, R. O. (2006) Atmospheres on the terrestrial planets clues to origin and evolution. Earth and Planetary Science Letters, 252, 1-14. 

Many asteroids are dry, as evidenced by meteorites in which water is virtually absent. These samples include many classes of chondrites, as well as melted chunks of the crusts, mantles, and cores of differentiated objects. Anhydrous bodies were important building blocks of the rocky terrestrial planets, and their chemical compositions reveal details of processes that occurred within our own planet on a larger scale. The distributions of these asteroids within the solar system also provide insights into their formation and evolution. 

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. 

D. M. Hunten, Atmospheric evolution of the terrestrial planets. Science 259, 915-920 (1993) J. F. Kasting, Earth s early atmosphere. Science 259, 920-926 (1993) R. A. Berner, Atmospheric carbon dioxide levels over phanerozoic time. Science 249, 1382-1386 (1990) R. A. Berner, Paleozoic atmospheric CO2 importance of solar radiation and plant evolution. Science 261, 68-70 (1993). 

Pepin, R. O. (1991) On the origin and early evolution of terrestrial planet atmospheres and meteoritic volatiles. Icarus, 92, 2-79. 

Ringwood, A. E. Chemical evolution of the terrestrial planets. Geochim. cosmochim. Acta 30, 41 (1966). 

There is evidence from chondrites that the solar nebula was well mixed between 0.1 and 10 AU during its first several million years of the evolution, as shown by the homogeneity in concentrations of many isotopes of refractory elements (Boss 2004 Chapter 9). This is likely caused by the evaporation and recondensation of solids in the very hot inner nebula, followed by outward transport due to turbulent diffusion and angular momentum removal. Materials out of which terrestrial planets and asteroids are built have been heated to temperatures above 1300 K and are thus depleted in volatile elements. The inner solar nebula, with some exceptions, does not retain memories of the pristine interstellar medium (ISM) chemical composition (Palme 2001 Trieloff Palme 2006). 

The giant planets, especially Jupiter and Saturn, significantly influenced accretion in the inner Solar System, with important consequences for the properties of the terrestrial planets, described in Section 10.4.1. The influence of the giant planets is especially strong in the Asteroid Belt. Given that meteorites are our primary samples of primitive Solar System material, understanding the role of dynamical and collisional processes in the formation and evolution of the Asteroid Belt is of fundamental importance for theories of planet formation (Section 10.4.2). 

The elements of the chondritic meteorites, and hence of the terrestrial planets, were formed in previous generations of stars. Their relative abundances represent the result of the general chemical evolution of the galaxy, possibly enhanced by recent local additions from one or more specific sources just prior to collapse of the solar nebula —4.56 Gyr ago. A volumetrically minor, but nevertheless highly significant part of this chemical inventory, is comprised of radioactive elements, from which this age estimate is derived. The famihar long-lived radionuclides, such as Th, Rb, K, and others,... 

Kaula W. M. (1986) The interiors of the terrestrial planets their structure and evolution. In The Solar System (ed. M. G. Kivelson). Prentice-Hall, Englewood Chffs, NJ, pp. 78-93. 

Van Keken P. E. and Ballentine C. J. (1998) Whole-mantle versus layered mantle convection and the role of a high-viscosity lower mantle in terrestrial volatile evolution. Earth Planet. Sci. Lett. 156, 19-32. 

Ahrens T. J., O Keefe J. D., and Lange M. A. (1989) Formation of atmospheres during accretion of the terrestrial planets. In Origin and Evolution of Planetary and Satellite Atmospheres (eds. S. K. Atreya, J. B. Pollack, and M. S. Matthews). University of Arizona Press, Tucson, pp. 328—385. 

Sasaki S. and Tajika E. (1995) Degassing history and evolution of volcanic activities of terrestrial planets based on radiogenic noble gas degassing models. In Volatiles in the Earth and Solar System, AlP Conf. Proc. 341 (ed. K. A. Farley). AIP Press, New York, pp. 186-199. 

While considerations of the origin of planetary noble gases have been predominantly focused on those presently found in the atmosphere, noble gases still within the Earth provide further constraints about volatile trapping during planet formation. A wide range of noble-gas information for the Earth s mantle has been obtained from mantle-derived materials, and indicates that there are separate reservoirs within the Earth that have distinctive characteristics that were established early in Earth history. These must be included in comprehensive models of Earth volatile history. Also, data are now available for the atmospheres of both Venus and Mars, as well as from the interior of Mars, so that the evolution of Earth volatiles can be considered within the context of terrestrial-planet formation across the solar system. 

Mars. The combination of Viking in situ measurements and SNC meteorite data has provided a much more quantitative view of the present state and possible history of martian volatiles. Further progress requires greater precision for the atmospheric composition, more data on possible near-surface and mantle reservoirs, and further constraints on the conditions that affect the volatile evolution of all the terrestrial planets. 

Pepin R. O. (1989) On the relationship between early solar activity and the evolution of terrestrial planet atmospheres. In The Formation and Evolution of Planetary Systems, Space Tel Sci. Inst. Symp. Series 3 (eds. H. A. Weaver and L. Danly). Cambridge University Press, Cambridge, UK, pp. 55-74. 

Cockell C. S. (2000) The ultraviolet history of the terrestrial planets—implications for biological evolution. Planet. Space Sci. 48, 203 -214. 

The cratered surfaces of asteroids and terrestrial planets underscore the importance of impacts for the formation and evolution of the solar system. Early in the history of the solar system such collisions were the mechanism for accretion of planetesimals and finally the planets themselves [1], The effects of these still ongoing collisions are visible from the megascopic down to the submicroscopic length scale, i.e., they range from large impact craters and their ejecta blankets down to shock-metamorphic effects in minerals [2-4]. These effects form as a result of the interaction of strong shock waves with the affected solid matter. 

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