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Circumstellar Disk Studies with the EVLA

Circumstellar Disk Studies with the EVLA. Carl Melis UCLA/LLNL In collaboration with: Gaspard Duchêne, Holly Maness, Patrick Palmer, and Marshall Perrin. NASA/CXC/M.Weiss. Why study disks?. Star Formation. Disk material feeds young star through accretion.

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Circumstellar Disk Studies with the EVLA

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  1. Circumstellar Disk Studies with the EVLA Carl Melis UCLA/LLNL In collaboration with: Gaspard Duchêne, Holly Maness, Patrick Palmer, and Marshall Perrin Slide 1 (of 18) NASA/CXC/M.Weiss

  2. Why study disks? • Star Formation • Disk material feeds young star • through accretion. • Disks facilitate the removal of • stellar angular momentum. • Jets launched by accreting disk • material can impact star’s natal • environment. HH30/HST-WFPC2 Slide 2 (of 18)

  3. Why study disks? • Planet Formation and Evolution • Disk grains grow from interstellar • size to planetesimals and eventually • planets. • Disks are the end result of planet • and planetsimal collisions. • Disk material traces planets through • their interaction with grains. Slide 3 (of 18) -Pic/HST-STIS

  4. VLA Protoplanetary Disk Studies • Most aimed towards measuring grain growth through spectral indices. Herbig Ae/Be stars: Natta et al. (2004) Slide 4 (of 18)

  5. VLA Protoplanetary Disk Studies • Most aimed towards measuring grain growth through spectral indices.  = 0.7±0.1 • = 1.3±0.1 • Rodmann et al. (2006) showed growth to cm sizes and that 7 mm • emission is optically thin. Slide 5 (of 18)

  6. VLA Protoplanetary Disk Studies • Greaves et al. may have detected a proto-gas giant planet forming in the disk of • HL Tau with high angular resolution 7 mm observations using VLA+PT.  = 0.7±0.1 • = 1.3±0.1 Planet? Jet Slide 6 (of 18)

  7. VLA Protoplanetary Disk Studies • Wilner et al. show growth beyond cm sizes in the disk of TW Hya.  = 0.7±0.1 • = 1.3±0.1 Wilner et al. (2005) Hughes et al. (2007) Slide 7 (of 18) Wilner et al. (2000)

  8. The EVLA • Point source sensitivity for 12 hours on-source, 1 rms.  = 0.7±0.1 • = 1.3±0.1 Slide 8 (of 18)

  9. The EVLA • Q- and K-band receivers with 2 GHz bandwidth will be the first fully available!  = 0.7±0.1 • = 1.3±0.1 Slide 9 (of 18)

  10. EVLA Disks Orion • Protoplanetary Disks • Grain growth in a statistical sense as a function of time. • Complete samples of targets for a range of masses. • Several star forming regions, e.g.:  = 0.7±0.1 • = 1.3±0.1 CrA  Oph Taurus Slide 10 (of 18)

  11. EVLA Disks • Protoplanetary Disks • Probing the spatial distribution of large grains. • Large grains predicted to drift into host star on short timescales. • Incompatible with current observations! • Need to probe radial distribution of large grains.  = 0.7±0.1 • = 1.3±0.1 Johansen & Klahr (2005) Slide 11 (of 18) Brauer et al. (2007)

  12. EVLA Disks • Protoplanetary Disks • Probing the spatial distribution of large grains. • Grain growth and sedimentation are predicted to be intimately linked. • Observe edge-on disks with compact and extended array configurations to test this prediction.  = 0.7±0.1 • = 1.3±0.1 Slide 12 (of 18)

  13. EVLA Disks • Protoplanetary Disks • Molecules with EVLA spectral line studies. • Important opacity sources for giant planet atmospheres. • Materials necessary for life.  = 0.7±0.1 • = 1.3±0.1 slide courtesy Claire Chandler Slide 13 (of 18)

  14. EVLA Disks • Debris Disks • A new way to discover planets? Bigger Smaller >~7 mm ~3 mm ~10 m ~0.1 m HD 107146; Corder et al. (2009) Wyatt (2005) HD 32297; Maness et al. (2008) • Watch the pattern move! • Planet at 100 AU orbiting a 10 pc distant 2 M star moves ~100 mas in 1 year. Slide 14 (of 18) Vega; Wilner et al. (2002)

  15. EVLA Disks • Phoenix Giant Disks • A second chance for planets? H in TYC 4144 329 2; Melis et al. (2009) CO (3-2) in BP Psc; Zuckerman et al. (2008) Slide 15 (of 18)

  16. The EVLA-ALMA Strip: Star Formation Slide 16 (of 18)

  17. The EVLA-ALMA Strip: Disks Slide 17 (of 18)

  18. Conclusions • The EVLA will enable unprecedented studies of disks forming and interacting with planets. • Grain growth and sedimentation across the Hayashi tracks. • Protoplanets within disks. • Molecular gas and organic material in disks. • Planets perturbing debris in mature planetary systems. • Rebirth of planetary systems around Phoenix Giants. Slide 18 (of 18) NASA/JPL/CalTech

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