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) N. Calvet (Michigan) C. Dullemond (MPIA) T. Henning (MPIA) H. Linz (MPIA) J. Greaves (St. Andrews) A. Isella (Caltech) L. Perez (Caltech) A. Sargent (Caltech) L. Mundy (Maryland) S. Storm (Maryland) J. Lazio (JPL) L. Testi (ESO) L. Ricci (ESO) PI: C. Chandler (NRAO) 217th AAS Meeting, Seattle, January 2011

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

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  ~ -   diagnostic of max size if optically thin, R-J F  T  -(  + 2) 217th AAS Meeting, Seattle, January 2011 see Draine 2006 Rodmann et al. 2006 ISM grains “pebbles” 2  0  n(a) ~ a 3.5 compact spheres

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 217th AAS Meeting, Seattle, January 2011 NASA/JPL T. Pyle C. Dominik

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

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  217th AAS Meeting, Seattle, January 2011 –  ’s agree, mm fluxes don’t… – growth to larger sizes? different initial conditions? = 2 + 

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

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