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ALMA does Circumstellar Disks

ALMA does Circumstellar Disks. A User’s Perspective on Early Science and Beyond. David J. Wilner. Harvard-Smithsonian Center for Astrophysics. “ Protoplanetary ” to “Debris ”. Corder et al 2009; Greaves et al. 2005. McCaughrean et al. 1995; Burrows et al. 1996.

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ALMA does Circumstellar Disks

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  1. ALMA does Circumstellar Disks A User’s Perspective on Early Science and Beyond • David J. Wilner • Harvard-Smithsonian Center for Astrophysics

  2. “Protoplanetary” to “Debris” Corder et al 2009; Greaves et al. 2005 McCaughrean et al. 1995; Burrows et al. 1996 Andrews; et al., in prep Isella et al. 2007 Kalas et al. 2008; Marois et al. 20010 • ~1 to 10 Myr • gas and trace dust • dust sticking, growing into planetesimals • 0.001 to 0.1 MSun • ~10 Myr to Gyrs • dust and trace gas • planetesimals colliding, creating dust • <1 MMoon • What physics drives evolution? When, where, how do planets form? • ALMA images dust and gas at key long wavelengths0.3 to 9 mm 217th AAS Meeting, Seattle, January 2011

  3. ALMA: Large, Sensitive, Fast! muchdeeper individual spectro-imaging studies and statistical views SMA ALMA ALMA Early Science CARMA IRAM PdBI inspired by E. Rosolowsky 217th AAS Meeting, Seattle, January 2011

  4. Debris Disk Structure >15% of nearby stars small dust ≠ large dust 10’s are 1-10 mJy at 850 mm early science DS ~1 mJy/√min full ALMA 3x better and longer baselines star ALMA 4h casa simulation ALMA Early Science 4h casa simulation disk Nilsson et al. 2009 ALMA Wilner et al. 2011 βPic, A6V, 19 pc Chris Stark dusty KB model 217th AAS Meeting, Seattle, January 2011

  5. Protoplanetary Disk Dust 100’s at 150 pc 0.005 Msun~80 mJy, at 850 mm structure, holes, gaps, planets! 870 mm RY Tau hydro simulation 100 AU primary beam fwhm DG Tau Williams et al. 2005 • 1000’s within 1 kpc • reach 1-10 Myr clusters • mass evolution, statistics 5 AU at the limits of ALMA Wolf & D’Angelo 2005 Isella et al. 2010 CARMA 1.3 mm 217th AAS Meeting, Seattle, January 2011

  6. Protoplanetary Disk Gas physical conditions, chemistry, dispersal Oberg et al. 2011 • CO 2-1 DCO+, H2CO, N2H+, … • 10 Jy km/s 1 Jy km/s • early science DS ~0.05 Jy km/s /√min Aikawa 2006 217th AAS Meeting, Seattle, January 2011

  7. Protoplanetary Disk Gas (continued) CO 3-2 DCO+ 3-2 Charlie Qi 217th AAS Meeting, Seattle, January 2011

  8. Concluding Remarks ALMA offers unprecedented sensitivity at millimeter wavelengths already at start of Early Science many fundamental issues to address, e.g. circumstellar disks reach Solar System scales for 100’s to 1000’s of sources expect a lot of surprises ALMA 4h casa simulation 217th AAS Meeting, Seattle, January 2011

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