François Ménard - National Radio Astronomy … · On the origin of the « Horseshoes » seen by...
Transcript of François Ménard - National Radio Astronomy … · On the origin of the « Horseshoes » seen by...
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On the origin of the « Horseshoes » seen by ALMA in Transition Disks
François Ménard UMI-FCA, Chile and IPAG, Grenoble, France
Peggy Varnière – APC, Paris, France
Héloïse Méheut -- AIM, CEA-Saclay, France
Christophe Pinte – UMI-FCA, Chile and IPAG, Grenoble, France
Simon Casassus – U de Chile
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ALMA transformational science: Dust traps
To form a planet, dust needs to grow… a lot small particles do stick and grow Big bodies do collide and grow into planetesimals
We have a problem for «meter sizes» radial drift too fast… boulders don’t stay in disk long enough to
grow « passed » that barrier. Need a way to overcome
Pressure maxima and RWI have been proposed to serve as « dust traps » before
1996 Barge & Sommeira 1999 Lovelace et al. 2006 Varniere & Tagger 2009 Lyra et al. 2011 Regaly et al. … and the recent work by Birnstiel, Pinilla, Dullemond …
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Long-lived vortices do exist !
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Outline
ALMA continuum data for Transition Disks
The Rossby Wave Instability Calculation set-up
Results of calculations + qualitative comparison with data
Future prospects 12/04/13 2013 ROCKS - Waikoloa, HI 4
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I- What are Transition Disks ?
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Sketch from C. Espaillat
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I- Transition Disks with ALMA
HD 142527
Recall previous talks by Simon Casassus, Misato Fukagawa & Henning Avenhaus
Image courtesy of Hector Canovas (in prep. 2013)
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I- Transition Disks with ALMA
HD 142527
Band 7 data (cycle 0)
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Image credit: Misato Fukagawa et al.
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I- Transition Disks with ALMA
The « horseshoe » is located at the disk rim…
… where conditions are met for RWI to grow
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Casassus et al. (2012, 2013)
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I- Transition Disks with ALMA
A variety of them…
Here, IRS 48
See Nienke van der Marel’s talk on Friday Cycle 0
Band 9
UNDER EMBARGO !
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Image credit: N. van der Marel
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I- Transition Disks with ALMA
SR 21
See Laura Perez’ talk in a few minutes.
Band 9
Cycle 0
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Image credit: Laura Perez
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I- Properties of the Horseshoes
Contrast (in surface brightness) Wide range, from a few to ~100
For HD 142527 (from Casassus’ data set) Azimuthal extent
Wavelength dependent
Radial extent Unresolved with current array,
marginally in Band 9.
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II- The Rossby Wave Instability
2 quantities: Vorticity (curl v), density (Σ) New word: Vortensity = vorticity / density
Conditions will be met for RWI to develop at position of extremum in gradient of vortencity. Was used at boundaries of dead zones Here we use at Inner Rim of Transition Disks
In other words: Keplerian disks are good places to find large vorticity Transition disks are good places to find large density
gradient with pronounced extrema…
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II- The numerical set-up
A disk « similar » to the outer disk of HD 142527 is used
Surface density profile α r -1
Rim of Outer disk located at 130AU Sharp Surface density drop
Total disk mass: 0.1Msun Global G/D ratio = 100
Not true locally after RWI sets in
Central star mass: 2.0 Msun
grid for hydro calculations: 512 cells radially (between 30 and 350 AU) 128 cells in azimuth direction
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III- Results and Comparison
Gas structure is modified azimuthally by RWI. Long-lived vortex is created
At R ~ 135AU, inner edge
Survives several 100’s of orbits, as long as conditions are present
Rotates at ~keplerian period See Ataiee et al.
Gas density contrast of a factor of ~2.
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Gas Surface density map
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III- Adding dust to the gas.
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Gas Surface density map Dust: 10 μm
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III- Adding dust to the gas.
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Gas Surface density map Dust: 100 μm
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III- Adding dust to the gas.
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Gas Surface density map Dust: 1 mm
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III- Preparing for Radiative Transfer
2-fluid Hydro sims’ are combined to produce one single density grid. 1 gas profile 5 dust profiles
1,10,100,1mm,1cm
Interpolate in between to build complete dust population in each grid cell
Assuming amin, amax, & slope
3rd dimension is hydrostatic equiibrium
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800 AU
350AU
130AU
201 pixels
III- Synthetic images: 2,7 mm (band 3)
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Not convolved, resoluWon 4AU/pixel
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III- Synthetic images: 1,3 mm (band 6)
Describe how the Num. Sim’s are combined to produce one single dust grid.
Gas -> relax Include 1 dust -> relax (few oribits
only)
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III- Synthetic images: 850 µm (band 7)
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III- Synthetic images: 350 µm (band 10)
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III- Synthetic images: 2,7 mm (band 3)
Describe how the Num. Sim’s are combined to produce one single dust grid.
Gas -> relax Include 1 dust -> relax (few oribits
only)
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Not convolved, 4AU/pixel
9 MEarth of dust
0.1 MEarth of dust
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III- further comparison
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Images are convolved by round 0.4arcsec beam , DetecWon limit added : 0.05 mJy/beam
Band 6 Band 7
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III- Map of emissivity index
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III- Synthetic images: 1.6 µm (scattered light)
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IV- Wrapping up
For Transition disks observed with ALMA Hydro calculations of the Rossby Wave
Instability captured the broad features of the observations and their behaviour with frequency for an object similar to HD 142527 Contrast, azimuthal extent, emissivity
3D version of the calculations is underway
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IV- To do list (partial)
To confirm presence / role of RWI:
Behaviour with time RWI = ~ keplerian rotation Resonance with Planets will be different
Behaviour of « Horseshoes » with size of inner hole RWI expected to produce larger density asymetries
Estimate radial extent of vortex Use (A)symmetry of vortex and Emissivity maps
Broad range of wavelength needed
DATA FITTING will be required (not done here) need proper treatment of uv coverage
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