Circumstellar Disk Masses in Young Clusters
Rich clusters provide an opportunity to study the frequency and evolution of circumstellar disks around large numbers of stars spanning two or more decades in stellar mass. In collaboration with John Carpenter, I have used OVRO to determine the distribution of circumstellar masses in the central regions of the young NGC 2024 and Orion Nebula clusters ( Eisner & Carpenter 2003; 2006). We are currently using the enhanced sensitivity of the new SMA and CARMA interferometers to extend these studies to lower disk masses and improve our understanding of the "typical" protoplanetary disk in clustered environments. Recent observations of the Orion Nebula cluster (Eisner et al. 2008) showed that less than ten percent of systems appear capable of forming massive, Jovian planets. Since most stars appear to form in Orion-like environment, this suggests that most protoplanetary disks may lack the mass needed to form solar systems like ours.


Josh Eisner; April 14, 2008