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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?. - PowerPoint PPT Presentation
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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?
Greaves & Rice 2011
HL Tau
• Class I low-mass protostar with massive envelope
Kwon, Looney & Mundy 2011CARMA, 1.3mm, 0.15"
Welch et al. 2004BIMA, 1.4mm, 0.3"
HL Tau b
• high-resolution imaging of large dust in the radio
Greaves, Richards, Rice & Muxlow 2008VLA, 1.3cm, 0.08-0.11"
...revisited
• re-observed recently with EVLA (preliminary reduction)
courtesy Disks@EVLA, PI Claire Chandler
disc instability
• SPH simulation naturally forms 8MJup object at 75 AU (vs. ~10-14MJup at 65 AU observed)
instability trigger?
• XZ Tau flyby of HL Tau at ~600 AU, ~1600 years ago?
Anglada et al. 2007Ducourant et al. 2005
disc interaction
• SPH simulation of such an encounter
Forgan & Rice
disc perturbation
• recent image with SCUBA-2 at 450 m
Greaves, Gibb, Sibthorpe et al.450 m, 8"
future observations
• have test-time for Key Project PEBBLES with eMERLIN at 5cm – survey of dust discs at longest wavelength so far!