Disks around y oung Brown Dwarfs as critical testbeds for
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Disks around young Brown Dwarfs as critical testbeds for
models of dust evolution: an investigation with ALMA
Luca Ricci (CARMA Fellow, Caltech)Testi (ESO/Germany), Natta, Scholz (DIAS), de Gregorio-Monsalvo
(ESO/Chile)Isella, Carpenter (Caltech), Pinilla (ITA), Birnstiel (LMU)
ALMA (ESO/NAOJ/NRAO)/Kornmesser, Calcada (ESO)
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From dust to planets
NASA/ESA, L. Ricci
Dullemond
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From dust to planets
NASA/ESA, L. Ricci
Dullemond
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From dust to planetesimalsmm-grains with
low sticking efficiency mm-grains drift fast
toward the central star
dPgas / dr > 0 :Reverse motion of solids, trapped at
P-maxima
dPgas / dr < 0 :Vgas < Vsolids
1mm1mm
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Grain sizing from mm-SED slopeFν ~ ν2 κν ;Fν ~ να, κν ~
νβα ~ 2 + β
Dullemond, Birnstiel
RJ tail
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Grain sizing from mm-SED slopeFν ~ ν2 κν ;Fν ~ να, κν ~
νβα ~ 2 + β
Draine 06
β < 1 (α < 3) only if ~ mm pebbles
in the outer disk (R > 10 AU)
β~1.7
β~0.5
Dullemond, Birnstiel
RJ tail
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Ricci+ 2011 Ricci+ 2010
Grain growth: observational results
~ 100 Class II disks around young stars
- mm-grains in the outer regions of nearly all disks: grain growth is fast even in the outer disk, i.e. < 1 Myr
(Beckwith & Sargent 91, Testi+ 03, Wilner+ 05, Andrews & Williams 05, Rodmann+ 06, Lommen+ 07, Ricci+ 10a,10b,11,12, Guilloteau+ 11, Ubach+12, …)
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Models of dust evolution in disks- Time evolution of gas surface density & temperature
- Solids with different sizes acquire relative velocities, i.e. they collide
Collision outcome: Δvcoll
fragmentationcoagulation
> v frag<
vfrag
Rotation
Brau
er+
08, B
irnst
iel+
10
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Models of dust evolution in disks
Solid
size
Distance from the star
Disk structure ( Σd(r), T(r) )
Birn
stie
l+ 2
010
Disk Fluxes(dist, incl)
Dust composition (e.g. Pollack+ 94)
κλ (r)
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Data vs models: the role of drift“SMOOTH” DISK, SELF-SIMILAR Σgas(R)
Pinilla, LR + 2012, Birnstiel, LR + 2010
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Data vs models: the role of drift
Pinilla, LR + 2012, Birnstiel, LR + 2010
PRESSURE MAXIMA (A≈0.3Σ0, l≈Hp)
“SMOOTH” DISK, SELF-SIMILAR Σgas(R)
:):)
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Disks with P-maxima3D MHD simulations of MRI-turbulent disks (Uribe+ 2011)
10 100 10 100
(are the required physical conditions met in real disks? stability?) If there, ALMA should see them… (Pinilla, LR+ 2012)
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Disks with P-maxima: model predictions
T Tauri disks
BD disks?
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Disks with P-maxima: model predictions
BD disks?
T Tauri disks
(Pinilla,LR+ 13, submitted)
less coag. to mmfaster radial drift
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ALMA
Disks with P-maxima: model predictions
T Tauri disks
4 disks with 1 < F1mm < 10 mJy around BDs and VLMs
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Rho Oph 102
MBD ≈ 60 MJup , Age ~ 1 Myr
Rho Oph 102
ESO/Digitized Sky Survey 2
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The disk around the young BD rho Oph 102
ALMA 0.89mm ALMA 3.2mm
α
rms = 0.04 mJy rms = 0.3 mJy
ALMA 0.89mm ALMA 3.2mm
Ricci + 12
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The disk around the young BD rho Oph 102
ALMA 0.89mm ALMA 3.2mm
rms = 0.04 mJy/b rms = 0.3 mJy/b
~ 30 min ALMA time~ 15 min ALMA time
Ricci + 12
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The disk around the young BD rho Oph 102
~ 15 min ALMA time ~ 30 min ALMA timevs ~ 500 hrs SMA time! vs ~ 120 hrs CARMA time!
ALMA 0.89mm ALMA 3.2mm
Ricci + 12
rms = 0.3 mJy/brms = 0.04 mJy/b
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The disk around the young BD rho Oph 102
CO (J = 3 - 2)
Cold Molecular gas from the disk
ALMA 0.89mm ALMA 3.2mm
rms = 0.04 mJy rms = 0.3 mJy
ALMA 0.89mm ALMA 3.2mm
gas-rich disk as in T Tauri disks
Ricci + 12
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2M0444+2512
FCRAO, G. Narayanan / M. HeyerMBD ≈ 50 MJup , Age ~ 1 Myr
2M0444
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The disk around the young BD 2M0444
α
ALMA 0.89mm ALMA 3.2mm
rms = 0.02 mJy/b rms = 0.4 mJy/b
Ricci + 13b, in prep
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The disk around the young BD 2M0444
CO (J = 3 - 2)4 km/s 7 km/s5 km/s 6 km/s 9 km/s8 km/s
Gas in rotation around the BD
Moment 1
Ricci + 13b, in prep
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The disk around the young BD 2M0444
Ricci + 13a
θ ≈ 0.15 arcsec, 10 AU in R
R > 10 AU
CARMA 1.3mm
CARMA 1.3mmVisibility vs Baseline
Dust optically thin: α ~ 2 + β
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ALMA
Disks with P-maxima: model predictions
T Tauri disks
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Disks with P-maxima: model predictions
T Tauri disks
rho Oph 102
Grain growth even in the outer regions of BD disks
CIDA-1CFHT-4
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Grain growth in BD disks: possible solution
Pinilla, LR + 13, submitted
- Disk outer radii ~ 15 – 30 AU- Low turbulent velocities α < 10-3
- Strong pressure bumps
(see also F. Meru’s poster)
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Grain growth in BD disks: possible solution
- Disk outer radii ~ 15 – 30 AU- Low turbulent velocities α < 10-3
- Strong pressure bumps
θ ~ 0.2 – 0.4’’
Modeling of molecular lines
B > 10 km
Pinilla, LR + 13, submitted
(see Dartois+03 Hughes+ 11, Guilloteau+ 12)
(see also F. Meru’s poster)
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Take away messages
- Grain growth to mm-sizes is fast (< 1 Myr) in both T Tauri and BD disks
- Dust trapping to explain mm-data of disks, ALMA should see the traps [trapping in transitional disks is from the P bump in the inner disk, here we are invoking trapping in the outer regions of primordial disks] - BD disks to test dust evolution models
- We started to probe dust properties and CO in BD disks: more to come in ALMA-Cycle 1 [see also Van der Plas poster]
[see Perez review talk on radial variation of β]