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Timescales of Disk Evolution and Planet Formation

Published online by Cambridge University Press:  26 May 2016

Ray Jayawardhana
Ray Jayawardhana*
Affiliation:
Department of Astronomy, University of California, Berkeley, CA 94720, U.S.A.

Abstract

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It has been suggested that circumstellar disks evolve from dense, actively accreting structures to low-mass, replenished remnants. During this transition, grains may assemble into planetesimals, or the disk may be cleared by newborn planets. Recently identified nearby groups of young stars provide valuable laboratories for probing disk evolution. I discuss the properties of dust disks in the TW Hydrae Association and the MBM 12 cloud, and compare the results to other studies of disk evolution and planet formation timescales.

Type
Part II: Progress in the theory of planet formation
Information
Symposium - International Astronomical Union , Volume 202: Planetary Systems in the Universe – Observation, Formation and Evolution , 2004 , pp. 196 - 198
Copyright
Copyright © Astronomical Society of the Pacific 2004 

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