Early evolution of the solar system: a geochemical perspective

Mathematics – Logic

Scientific paper

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Scientific paper

Timescales for the earliest processes in the solar system can be inferred from various formation and evolution models of the proto-solar nebula, from theoretical calculations and dynamic simulations, and from observations of circumstellar disks and planets. However precise chronological constraints do not come from models and simulations but are obtained on real objects that experienced these events, hence the interest of meteorites that can be studied in the laboratory. Their geochemical properties and isotopic composition provide various key informations about the accretion, differentiation and early evolution of their parent bodies and about the exact timescales of the processes. To date these events, natural radioactive isotopes are used. While chronometers based on long-lived radionuclides (206Pb-207Pb, 147Sm-143Nd, 87Rb- 87Sr) provide absolute ages, extinct radioactivities (182Hf-182W, 53Mn-53Cr, 26Al- 26Mg, . . . ) only give relative ages but with a high precision (typically better than 0.1 Ma) due to the short half-life of the parent isotope (t1/2 < 100 Ma). Isotopic systems not only register planetary, but also nebular processes. Isotopes also bring contraints on the stellar environment around the young Sun, on the time interval between the last nucleosynthetic event that delivered matter to the nebula and the formation of the first solid objects in the solar system, on the homogeneity of the solar nebula, and on the possible heat sources at the origin of the melting and differentiation of many planetesimals. In fact, radioactive systems as a whole help constrain the different evolution models of the early solar system because they have at one and the same time different physico-chemical properties and characteristic half-lives that permit to look at different timescales.

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