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Dust Chemistry and Dynamics in the Solar Nebula


IPGP - Îlot Cuvier


Séminaires de Géophysique expérimentale

Salle 108

Francesco Pignatale

UCB Lyon

Planets, meteorites and comets all result from different physical, chemical and dynamical processes which occurred during the protoplanetary disc phase of our Solar System. Among these objects, meteorites like carbonaceous and enstatite chondrites represent the most puzzling and dust dynamics clearly played an important role in their formation. Furthermore, the presence of CAIs in carbonaceous chondrites and refractory dust in cometary samples suggest that an efficient outward transport of grains occurred at the early stages of our Solar System formation. To date, there is no consensus on the processes which formed all these objects. Thus, in order to understand the story of meteorites and comets, a simultaneous approach to determine the chemistry and dynamics of the dust in the Solar Nebula is needed. In the first part of this talk I will present our approach to determine the 2D dust chemical distribution within the Solar Nebula and clues on the formation of enstatite chondrites. In the second part of the talk I will focus on 3D-SPH simulations performed to investigate the dynamics (settling, fractionation, sorting and radial migration of grains) of dust with different chemical composition, showing that dust sorting and fractionation are efficient processes in disks and may actually account for the formation of the bulk composition of enstatite chondrites. In the last part of the talk I will present results from preliminary tests of 3D-SPH simulations of magnetic driven Jet-flow as a possible mechanism of outward transport of refractory grains in the Solar Nebula.