Disk Dispersal and Planet Formation Time Scales

Abstract

Well before the existence of exo-solar systems was confirmed, it was accepted knowledge that most -- if not all -- stars possess circumstellar material during the first one-to-several million years of their pre-main sequence lives, and thus that they commonly have the potential to form planets. Here I summarize current understanding regarding the evolution of proto-planetary dust and gas disks, emphasizing the diversity in evolutionary paths.

Similar to version that will be published by IOP in 2008, Physica Scripta (Special Issue on Nobel Symposium 135: Physics of Planetary Systems)

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