Physics
Scientific paper
Dec 2010
adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2010agufm.v43d..01m&link_type=abstract
American Geophysical Union, Fall Meeting 2010, abstract #V43D-01
Physics
[1027] Geochemistry / Composition Of The Planets, [1040] Geochemistry / Radiogenic Isotope Geochemistry, [1060] Geochemistry / Planetary Geochemistry, [5405] Planetary Sciences: Solid Surface Planets / Atmospheres
Scientific paper
The solar system formation starts by a flared planetary disk of few hundred of AU composed of gas and 1% dust. Dust falls to the equatorial disk and migrate to the central star. During this stage, grains suffer an important radial and vertical transport. Because of turbulence, dust is thought to experience a strong vertical mixing. Therefore grains see different thermodynamical conditions (e.g. P, T, Solar irradiation) depending on their size and location. The next stage of solar system formation is the agglomeration of these grains to form macroscopic solids and in less than 100My, planets. We propose that during the “dust stage” of the solar system formation, the grains are submitted to a solar wind irradiation, which allows the incorporation of important quantities of rare gases in parent bodies, with solar-like isotopic compositions. Ion implantation is a mass fractionation process and the result of the solar-wind implantation leads to He-Ne-Ar isotopic ratios similar to the Earth noble gas isotopic ratios [Raquin and Moreira, EPSL 287 (2009) 551-558]. Furthermore, heavy rare gases (Kr, Xe) can also follow cycles of adsorption-desorption on dust of solar gas, a process that could fractionate isotopes in presence of UV. Such isotopic fractionation has been observed in laboratory experiments and gives isotopic compositions of Kr and Xe similar to the Earth's atmosphere and mantle when starting from solar compositions. In this scenario, volatiles were within Earth’s parent bodies and at least for rare gases, there is no need for a late bombardment. Direct 3D numerical simulations of dust transport in the turbulent protoplanetary disk will also be discussed to assess the plausibility of this scenario.
Charnoz Sebastien
Milesi V.
Moreira Anamaria Martins
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