Protoplanetary disks Jonathan Williams Institute for Astronomy University

Protoplanetary disks Jonathan Williams Institute for Astronomy, University of Hawaii Smithsonian Jes Jorgensen, David Wilner JCMT CA Doug Johnstone JCMT NL Sandrine Bottinelli, Michiel Hogerheijde, Dave Lommen, Olja Panic, Demerese Salter, Ronald Stark, Ewine van Dishoeck JCMT UK Bill Dent, Jason Kirk, John Richer Caltech Geoff Blake

http: //astro. berkeley. edu/~kalas

Disks are… the last step in the transport of the ISM to stellar scales And they are bright, compact objects, perfectly suited for interferometry! the first step in the formation of planetary systems

Strawman proposal • Disk formation • Disk structure • Chemistry • Environment • Debris

Strawman proposal • Disk formation • Disk structure ~0. 3” ~0. 5 km angular resolution baseline lengths ~ 200 AU 1 -2” ~100 m

DISK FORMATION

Embedded disks: motivation Angular mtm conservation rapid disk growth, R ~ t 3 But the disk is embedded in a bright CS envelope Note: early results with the JCMT-CSO interferometer (Lay et al. 1994; Brown et al. 2000)

Embedded disks: previous results Envelope (constrained through SCUBA observations; Jørgensen et al. (2002)) Disk (resolved) 0. 3 Jy @ > 150 k …the SMA resolves the warm dust in the inner envelope Extended structure Higher resolution and the (300 AU diameter) circumstellar disk. Jørgensen et al. 2005, Ap. J, 632, 973

Embedded disks: previous results Separation of envelope and disk chemistry? Jorgensen et al. 2005

Embedded disks: caveats • Small scale envelope structure • Outflows • Multiplicity need well characterized sources Looney et al. 2000

Embedded disks: sample ALSO MAY WANT TO CONSIDER CLASS I DISKS

Embedded disks: time estimate The 10 PROSAC candidate embedded disks are bright (> 0. 1 Jy) and unresolved (<2’’) could image >1 source per track? 5 -10 tracks for program +30 o Extended SMA +JCMT+CSO (but good uvcoverage essential)

DISK STRUCTURE

Disk structure: motivation • Transition disks show disks disperse and may signpost protoplanets • Radial density structure constrains planet formation models • Azimuthal variations

Transition disks: previous results The transition disk GM Aur SED dip inner hole out to ~24 AU (Calvet et al. 2005)

Transition disks: previous results Simulated observation Model based on SED

Transition disks: previous results Simulated observation SMA observations 0. 21’’x 0. 24’’ Wilner et al. 2007(? )

Transition disks: previous results 1. 5 tracks; Brown & Blake 2007(? )

Transition disks: sample Ask Geoff! “ 10+ systems” + several well known examples: GM Aur TW Hya DM Tau Lk Ca 15 Co. Ku Tau/4

Transition disks: time estimate Based on SMA obs of GM Aur and Lk. H 330, need 1 “good” track per source(? ) 10 tracks for program +60 o Very extended SMA +JCMT+CSO

Radial structure SMA e. SMA Andrews & Williams 2007 (astro-ph/0610813)

Azimuthal structure Lin et al. 2006

Other considerations • Are CARMA and Pd. BI collaborative or competitive? • Can the science be done with the SMA alone?

SUMMARY • Determine disk sizes at early times • Image inner holes of transition disks • Constrain radial density profiles into planet forming region • Explore azimuthal variations

Additional topics (2 nd year? )

Chemistry Charlie Qi thesis

SMA 880µm observations of the Trapezium Cluster ~0. 1 pc 0. 019 M 0. 016 M 0. 024 M 0. 013 M Williams, Andrews, & Wilner 2005 Protoplanetary disks capable of forming solar system scale architectures exist in massive star forming regions

Debris disks Williams et al. 2005