Disk Processes in the Formation of the Solar System

Date & time

12.30–1.30pm 6 October 2017


Ringwood Room, J4


Trevor Ireland (RSES)


 Michael Anenburg
 0451 406 232

Meteorites provide us with a glimpse into the formation of our solar system 4,567 to 4,558 million years (Myr) ago.  This was an epoch of high temperature fractionation of ultra-refractory elements, gas-solid reactions, condensation and evaporation, melting and remelting of refractory objects, accretion, and ultimately planet building.  A major difficulty in understanding the thermal history of the solar system is placing the objects under investigation in to spatial and temporal context.  While we are making gains in terms of temporal constraints, there is little to help us identify the specific context of meteoritic inclusions.

Observations of exo-planetary systems are beginning to inform us about the context of star and planet formation.   Observations of young stellar systems indicate that discs are cleared within 10 Myr.  Formation of refractory inclusions and chondrules must have occurred early in a very dust rich environment.  In this era, young stellar objects are redistributing angular momentum to allow material to fall in to the star.  Magneto-centrifugally accelerated bi polar jets provide a likely scenario for transporting angular momentum away from the young stars.  Extension of magnetic winds in to the disk offers a mechanism of producing high temperatures that would allow fractionation of ultrarefractory elements and also substantial metal-silicate fractionation.  A disc wind would lead to the devolatilisation of the inner solar system apparent in the composition of the terrestrial planets.

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