Differentiation of Planetesimals and the Thermal Consequences of Melt Migration

Details Differentiation of Planetesimals and the Thermal Consequences of Melt Migration Differentiation of Planetesimals and the Thermal Consequences of Melt Migration

2011-01-21

arxiv.org/abs/1101.4165v1

Astronomy and Astrophysics

Astrophysics

Earth and Planetary Astrophysics

33 pages, 5 figures, accepted to Meteoritics and Planetary Science

Scientific paper

We model the heating of a primordial planetesimal by decay of the short-lived radionuclides Al-26 and Fe-60 to determine (i) the timescale on which melting will occur; (ii) the minimum size of a body that will produce silicate melt and differentiate; (iii) the migration rate of molten material within the interior; and (iv) the thermal consequences of the transport of Al-26 in partial melt. Our models incorporate results from previous studies of planetary differentiation and are constrained by petrologic (i.e. grain size distributions), isotopic (e.g. Pb-Pb and Hf-W ages) and mineralogical properties of differentiated achondrites. We show that formation of a basaltic crust via melt percolation was limited by the formation time of the body, matrix grain size and viscosity of the melt. We show that low viscosity (< 1 Pa-s) silicate melt can buoyantly migrate on a timescale comparable to the mean life of Al-26. The equilibrium partitioning of Al into silicate partial melt and the migration of that melt acts to dampen internal temperatures. However, subsequent heating from the decay of Fe-60 generated melt fractions in excess of 50%, thus completing differentiation for bodies that accreted within 2 Myr of CAI formation (i.e. the onset of isotopic decay). Migration and concentration of Al-26 into a crust results in remelting of that crust for accretion times less than 2 Myr and for bodies >100 km in size. Differentiation would be most likely for planetesimals larger than 20 km in diameter that accreted within ~2.7 Myr of CAI formation.

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