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Rocky bodies of the inner solar system display a systematic depletion of the"Moderately Volatile Elements" (MVEs) that correlates with the expectedcondensation temperature of their likely host materials under protoplanetarynebula conditions. In this paper, we present and test a new hypothesis in whichopen system loss processes irreversibly remove vaporized MVEs from high nebulaaltitudes, leaving behind the more refractory solids residing much closer tothe midplane. The MVEs irreversibly lost from the nebula through these opensystem loss processes are then simply unavailable for condensation ontoplanetesimals forming even much later, after the nebula cooled, overcoming acritical difficulty encountered by previous models of this type. We model opensystem loss processes operating at high nebula altitudes, such as resultingfrom disk winds flowing out of the system entirely, or layered accretiondirectly onto the young sun. We find that mass loss rates higher than found intypical T-Tauri disk winds, lasting short periods of time, are mostsatisfactory, pointing to multiple intense early outburst stages. Using ourglobal nebula model, incorporating realistic particle growth and inward driftfor solids, we constrain how much the MVE depletion signature in the innerregion is diluted by the drift of undepleted material from the outer nebula. Wealso find that a significant irreversible loss of the common rock-formingelements (Fe, Mg, Si) can occur, leading to a new explanation of anotherlongstanding puzzle of the apparent "enhancement" in the relative abundance ofhighly refractory elements in chondrites.

Depletion of Moderately Volatile Elements by Open-System loss in the Early Solar Nebula