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Exploring Protoplanetary Disks with EVLA: Insights into Star and Planet Formation

This study presents new findings on protoplanetary disks utilizing the Enhanced Very Large Array (EVLA). Disks are vital to understanding star formation, as they provide material through accretion, while also facilitating stellar angular momentum removal. We investigate grain growth dynamics, the formation of planetesimals, and the impact of accreting material on a star's environment. Our research highlights the significance of disk studies in shedding light on the processes that lead to planet formation and the evolution of planetary systems, including insights from multiple star-forming regions.

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Exploring Protoplanetary Disks with EVLA: Insights into Star and Planet Formation

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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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