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Protoplanetary disks

Protoplanetary disks. Jonathan Williams Institute for Astronomy, University of Hawaii. http://astro.berkeley.edu/~kalas. And they are bright, compact objects, perfectly suited for interferometry!. Disks are… the last step in the transport of the ISM to stellar scales.

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Protoplanetary disks

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  1. Protoplanetary disks Jonathan Williams Institute for Astronomy, University of Hawaii

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

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

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

  5. angular resolution ~0.3” 1-2” ~0.5 km ~100 m baseline lengths ~ 200 AU Strawman proposal • Disk formation • Disk structure

  6. DISK FORMATION

  7. Embedded disks: motivation • Angular mtm conservation • rapid disk growth, R ~ t3 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)

  8. Envelope (constrained through SCUBA observations; Jørgensen et al. (2002)) Disk (resolved) Extended structure Higher resolution Embedded disks: previous results 0.3 Jy @ > 150k …the SMA resolves the warm dust in the inner envelope and the (300 AU diameter) circumstellar disk. Jørgensen et al. 2005, ApJ, 632, 973

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

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

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

  12. 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 (but good uv-coverage essential) +30o Extended SMA +JCMT+CSO

  13. DISK STRUCTURE

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

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

  16. Transition disks: previous results Simulated observation Model based on SED

  17. Transition disks: previous results Simulated observation SMA observations 0.21’’x0.24’’ Wilner et al. 2007(?)

  18. Transition disks: previous results 1.5 tracks; Brown & Blake 2007(?)

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

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

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

  22. Azimuthal structure Lin et al. 2006

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

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

  25. Additional topics (2nd year?)

  26. Chemistry Charlie Qi thesis

  27. Protoplanetary disks capable of forming solar system scale architectures exist in massive star forming regions 0.019 M ~0.1 pc 0.016 M 0.024 M 0.013 M SMA 880µm observations of the Trapezium Cluster Williams, Andrews, & Wilner 2005

  28. Debris disks Williams et al. 2005

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