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Disks@EVLA

Disks@EVLA. Grain Growth and Substructure in Protoplanetary Disks. David J. Wilner. Harvard-Smithsonian Center for Astrophysics. S. Corder (NRAO) A. Deller (NRAO) S. Andrews ( CfA ) D. Wilner ( CfA ) J. Carpenter (Caltech). A. Isella (Caltech) L. Perez (Caltech)

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Disks@EVLA

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  1. Disks@EVLA Grain Growth and Substructure in Protoplanetary Disks David J. Wilner Harvard-Smithsonian Center for Astrophysics S. Corder (NRAO) A. Deller (NRAO) S. Andrews (CfA) D. Wilner (CfA) J. Carpenter (Caltech) A. Isella (Caltech) L. Perez (Caltech) A. Sargent (Caltech) L. Mundy (Maryland) S. Storm (Maryland) N. Calvet (Michigan) C. Dullemond (MPIA) T. Henning (MPIA) H. Linz (MPIA) J. Greaves (St. Andrews) J. Lazio (JPL) L. Testi (ESO) L. Ricci (ESO) PI: C. Chandler (NRAO) 217th AAS Meeting, Seattle, January 2011

  2. From Dust to Planets star disk T Tauri & HAe stars age 1-10 Myr 100’s at ~140 pc NASA/JPL T. Pyle Planetesimal formation Planet formation Gravity- assisted growth Gas capture Collisionalagglomoration ??? (collective effects) 1mm 1mm 1m 1km 1000km 217th AAS Meeting, Seattle, January 2011

  3. Protoplanetary Disk Dust Emission • mm/cm wavelengths • avoid high opacities mass tracer • sensitive to cold dust including mid-plane • sensitive to large dust grain growth • contrast with star planet-forming region • subarcsec imaging with high sensitivity EVLA! • sometimes ionized gas 217th AAS Meeting, Seattle, January 2011

  4. Spectral Signatures of Growth mm/cm emissivity ~ l- b diagnostic of max size if optically thin, R-J F ~  S T ~ l-(b+ 2) 0 n(a) ~ a3.5 compact spheres 2 b see Draine 2006 b ISM grains “pebbles” Rodmann et al. 2006 217th AAS Meeting, Seattle, January 2011

  5. EVLA Observations photometry survey D/DnC/C arrays, ongoing 60+ nearby disks at 7/9/13/50 mm spectral indices for grain growth statistics, e.g. star properties, environment image subsets at higher resolution, to 50 mas = few AU C/CnB/B/BnA/A arrays, coming soon locate large grains surface density structure evidence for disk-planet interactions C. Dominik NASA/JPL T. Pyle 217th AAS Meeting, Seattle, January 2011

  6. Example Taurus Images (Preliminary) l = 9 mm (30.5 and 37.5 GHz) θ~ 0.7 arcsec = 100 AU spectral indices 217th AAS Meeting, Seattle, January 2011

  7. Some Early Analysis compare with Birnstiel et al. 2010 models self-consistent calculation of grain size distribution, coagulation/fragmentation and irradiated disk structure predict mm/cm fluxes and spectral index b = 2 + b • b’s agree, mm fluxes don’t… • growth to larger sizes? different initial conditions? 217th AAS Meeting, Seattle, January 2011

  8. Resolved Disk Colors and Structure • disk-planet interactions? efficient grain growth at highest densities? EVLA simulation surface densities and initial conditions? TW Hya Hughes et al. 2007 Kokubo and Ida 2002 217th AAS Meeting, Seattle, January 2011

  9. Disks@EVLA: Summary grain growth and substructure in protoplanetary disks last observable link in chain from ISM to planets photometry of 60+ disks at 7/9/13/50 mm spectral indices reveal large grains reduction and modeling underway imaging of subsets, to 50 mas = few AU expect resolved mm/cm colors surface densities, disk-planet features thanks to EVLA commissioning team! 217th AAS Meeting, Seattle, January 2011

  10. 217th AAS Meeting, Seattle, January 2011

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