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imaging the candidate proto-planet HL Tau b

imaging the candidate proto-planet HL Tau b. Jane Greaves University of St Andrews Anita Richards, Tom Muxlow (Jodrell Bank Centre for Astrophysics) Ken Rice, Duncan Forgan, Bruce Sibthorpe (Edinburgh). growth phase. when does dust grow into (unobservable) planetesimals?.

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imaging the candidate proto-planet HL Tau b

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  1. imaging the candidate proto-planet HL Tau b Jane Greaves University of St Andrews Anita Richards, Tom Muxlow (Jodrell Bank Centre for Astrophysics) Ken Rice, Duncan Forgan, Bruce Sibthorpe (Edinburgh)

  2. growth phase • when does dust grow into (unobservable) planetesimals? Greaves & Rice 2011

  3. HL Tau • Class I low-mass protostar with massive envelope Kwon, Looney & Mundy 2011 CARMA, 1.3mm, 0.15" Welch et al. 2004 BIMA, 1.4mm, 0.3"

  4. HL Tau b • high-resolution imaging of large dust in the radio Greaves, Richards, Rice & Muxlow 2008 VLA, 1.3cm, 0.08-0.11"

  5. ...revisited • re-observed recently with EVLA (preliminary reduction) courtesy Disks@EVLA, PI Claire Chandler

  6. disc instability • SPH simulation naturally forms 8MJup object at 75 AU (vs. ~10-14MJup at 65 AU observed)

  7. instability trigger? • XZ Tau flyby of HL Tau at ~600 AU, ~1600 years ago? Anglada et al. 2007 Ducourant et al. 2005

  8. disc interaction • SPH simulation of such an encounter Forgan & Rice

  9. disc perturbation • recent image with SCUBA-2 at 450 m Greaves, Gibb, Sibthorpe et al. 450 m, 8"

  10. future observations • have test-time for Key Project PEBBLES with eMERLIN at 5cm – survey of dust discs at longest wavelength so far!

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