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Poster Blitz #41. Banzatti, A.2. Birnstiel, T.3. Carmona, A.4. Dougados, C. 5. Gonzalez, J.-F.6. Kamp, I.
7. Kluska, J.8. Lambrechts, M.9. Maaskant, K.10. Mathews, G.11. McClure, M.12. Mulders, G.
Illustration credit: ESO/L. Calçada
EX Lupi from Quiescence to Outburst: Opening a New Window on Chemistry and Dynamics of Volatile Species in Planet-Forming Circumstellar Disks.Presenter: A. Banzatti, Institute of Astronomy, ETH Zurich, Switzerland
Outburst
Quiescence
Models
strong HI , H2 appearorganics disappear OH increases, new lines appear
Observable Signatures of Dust EvolutionT. Birnstiel, S. Andrews, B. Ercolano, H. Klahr
observed gas
observed dust
predicted dust(without cutoff)
also on the poster:
„Can grain growth explain
transitional disks?“
fragmentation
radial drift
effective in inner regions ⇒ MMSN
effective in outer regions, see figure/ r�0.75⌃dust
/ r�1.5⌃dust
⇒⇒
Employing H2 near-IR lines to understand the circumstellar environment of sources with
Spitzer [Ne II] 12.8 micron emission
★ What is circumstellar environment of the sources with Spitzer [Ne II] emission?
★ Ongoing CRIRES R~90000 survey for H2 near-IR emission in sources with the [Ne II] line
★ 8 of 18 objects observed: 4 detections H2 1-0 S(1) line
A. Carmona (Grenoble), M. Audard (Geneva), C. Baldovin-Saavedra (Geneva), M. Güdel (Vienna), J. Bary (Colgate)
disk
low velocity outflow
Simultaneous modeling of gas and dust diagnostics in the circumstellar disk of
HD135344B
A. Carmona (Grenoble), C. Pinte (Grenoble), W.F. Thi (Grenoble), M. Benisty (Grenoble), F. Menard (Grenoble) + GASPS collaboration
A. Carmona et al.: Understanding the circumstellar disk of HD135344B by multiwavelength observations and modeling
Model 33 Model 34 Model 46
[OI] 63.18µm
10-810-610-410-2100102
o
oline
ocont
0
20406080
100
0cum
ulat
ive
F line [%
] Fline
= 6.58E-17 W/m2
0.1 1.0 10.0 100.0r [AU]
0.00.2
0.4
0.6
0.8
1.0
z/r
0 2 4 6 8log n
O [cm-3]
[OI] 63.18µm
10-810-610-410-2100102
o
oline
ocont
0
20406080
100
0cum
ulat
ive
F line [%
] Fline
= 6.76E-17 W/m2
0.1 1.0 10.0 100.0r [AU]
0.00.2
0.4
0.6
0.8
1.0
z/r
0 2 4 6 8log n
O [cm-3]
[OI] 63.18µm
10-810-610-410-2100102
o
oline
ocont
0
20406080
100
0cum
ulat
ive
F line [%
] Fline
= 4.47E-17 W/m2
1 10 100r [AU]
0.00.20.40.60.81.01.2
z/r
0 2 4 6 8log n
O [cm-3]
CO 866.96µm
10-610-410-2100102104
o
oline
ocont
0
20406080
100
0cum
ulat
ive
F line [%
] Fline
= 1.32E-19 W/m2
0.1 1.0 10.0 100.0r [AU]
0.00.2
0.4
0.6
0.8
1.0
z/r
-6 -4 -2 0 2 4 6log n
CO [cm-3]
CO 866.96µm
10-610-410-2100102104
o
oline
ocont
0
20406080
100
0cum
ulat
ive
F line [%
] Fline
= 1.33E-19 W/m2
0.1 1.0 10.0 100.0r [AU]
0.00.2
0.4
0.6
0.8
1.0
z/r
-6 -4 -2 0 2 4 6 8log n
CO [cm-3]
CO 866.96µm
10-610-410-2100102104
o
oline
ocont
0
20406080
100
0cum
ulat
ive
F line [%
] Fline
= 1.44E-19 W/m2
1 10 100r [AU]
0.00.20.40.60.81.01.2
z/r
-6 -4 -2 0 2 4 6 8log n
CO [cm-3]
CO 4.844µm
10-810-610-410-2100102
o
oline
ocont
0
20406080
100
0cum
ulat
ive
F line [%
] Fline
= 1.15E-17 W/m2
0.1 1.0 10.0 100.0r [AU]
0.00.2
0.4
0.6
0.8
1.0
z/r
-6 -4 -2 0 2 4 6log n
CO [cm-3]
CO 4.844µm
10-810-610-410-2100102
o
oline
ocont
0
20406080
100
0cum
ulat
ive
F line [%
] Fline
= 1.46E-17 W/m2
0.1 1.0 10.0 100.0r [AU]
0.00.2
0.4
0.6
0.8
1.0
z/r
-6 -4 -2 0 2 4 6 8log n
CO [cm-3]
CO 4.844µm
10-610-410-2100102104
o
oline
ocont
0
20406080
100
0cum
ulat
ive
F line [%
] Fline
= 2.81E-17 W/m2
1 10 100r [AU]
0.00.20.40.60.81.01.2
z/r
-6 -4 -2 0 2 4 6 8log n
CO [cm-3]
Fig. 1.
5
A. Carmona et al.: Understanding the circumstellar disk of HD135344B by multiwavelength observations and modeling
Model 33 Model 34 Model 46
[OI] 63.18µm
10-810-610-410-2100102
o
oline
ocont
0
20406080
100
0cum
ulat
ive
F line [%
] Fline
= 6.58E-17 W/m2
0.1 1.0 10.0 100.0r [AU]
0.00.2
0.4
0.6
0.8
1.0
z/r
0 2 4 6 8log n
O [cm-3]
[OI] 63.18µm
10-810-610-410-2100102
o
oline
ocont
0
20406080
100
0cum
ulat
ive
F line [%
] Fline
= 6.76E-17 W/m2
0.1 1.0 10.0 100.0r [AU]
0.00.2
0.4
0.6
0.8
1.0
z/r
0 2 4 6 8log n
O [cm-3]
[OI] 63.18µm
10-810-610-410-2100102
o
oline
ocont
0
20406080
100
0cum
ulat
ive
F line [%
] Fline
= 4.47E-17 W/m2
1 10 100r [AU]
0.00.20.40.60.81.01.2
z/r
0 2 4 6 8log n
O [cm-3]
CO 866.96µm
10-610-410-2100102104
o
oline
ocont
0
20406080
100
0cum
ulat
ive
F line [%
] Fline
= 1.32E-19 W/m2
0.1 1.0 10.0 100.0r [AU]
0.00.2
0.4
0.6
0.8
1.0
z/r
-6 -4 -2 0 2 4 6log n
CO [cm-3]
CO 866.96µm
10-610-410-2100102104
o
oline
ocont
0
20406080
100
0cum
ulat
ive
F line [%
] Fline
= 1.33E-19 W/m2
0.1 1.0 10.0 100.0r [AU]
0.00.2
0.4
0.6
0.8
1.0
z/r
-6 -4 -2 0 2 4 6 8log n
CO [cm-3]
CO 866.96µm
10-610-410-2100102104
o
oline
ocont
0
20406080
100
0cum
ulat
ive
F line [%
] Fline
= 1.44E-19 W/m2
1 10 100r [AU]
0.00.20.40.60.81.01.2
z/r
-6 -4 -2 0 2 4 6 8log n
CO [cm-3]
CO 4.844µm
10-810-610-410-2100102
o
oline
ocont
0
20406080
100
0cum
ulat
ive
F line [%
] Fline
= 1.15E-17 W/m2
0.1 1.0 10.0 100.0r [AU]
0.00.2
0.4
0.6
0.8
1.0
z/r
-6 -4 -2 0 2 4 6log n
CO [cm-3]
CO 4.844µm
10-810-610-410-2100102
o
oline
ocont
0
20406080
100
0cum
ulat
ive
F line [%
] Fline
= 1.46E-17 W/m2
0.1 1.0 10.0 100.0r [AU]
0.00.2
0.4
0.6
0.8
1.0
z/r
-6 -4 -2 0 2 4 6 8log n
CO [cm-3]
CO 4.844µm
10-610-410-2100102104
o
oline
ocont
0
20406080
100
0cum
ulat
ive
F line [%
] Fline
= 2.81E-17 W/m2
1 10 100r [AU]
0.00.20.40.60.81.01.2
z/r
-6 -4 -2 0 2 4 6 8log n
CO [cm-3]
Fig. 1.
7
A. Carmona et al.: Understanding the circumstellar disk of HD135344B by multiwavelength observations and modeling
Model 33 Model 34 Model 46
[OI] 63.18µm
10-810-610-410-2100102
o
oline
ocont
0
20406080
100
0cum
ulat
ive
F line [%
] Fline
= 6.58E-17 W/m2
0.1 1.0 10.0 100.0r [AU]
0.00.2
0.4
0.6
0.8
1.0
z/r
0 2 4 6 8log n
O [cm-3]
[OI] 63.18µm
10-810-610-410-2100102
o
oline
ocont
0
20406080
100
0cum
ulat
ive
F line [%
] Fline
= 6.76E-17 W/m2
0.1 1.0 10.0 100.0r [AU]
0.00.2
0.4
0.6
0.8
1.0
z/r
0 2 4 6 8log n
O [cm-3]
[OI] 63.18µm
10-810-610-410-2100102
o
oline
ocont
0
20406080
100
0cum
ulat
ive
F line [%
] Fline
= 4.47E-17 W/m2
1 10 100r [AU]
0.00.20.40.60.81.01.2
z/r
0 2 4 6 8log n
O [cm-3]
CO 866.96µm
10-610-410-2100102104
o
oline
ocont
0
20406080
100
0cum
ulat
ive
F line [%
] Fline
= 1.32E-19 W/m2
0.1 1.0 10.0 100.0r [AU]
0.00.2
0.4
0.6
0.8
1.0
z/r
-6 -4 -2 0 2 4 6log n
CO [cm-3]
CO 866.96µm
10-610-410-2100102104
o
oline
ocont
0
20406080
100
0cum
ulat
ive
F line [%
] Fline
= 1.33E-19 W/m2
0.1 1.0 10.0 100.0r [AU]
0.00.2
0.4
0.6
0.8
1.0
z/r
-6 -4 -2 0 2 4 6 8log n
CO [cm-3]
CO 866.96µm
10-610-410-2100102104
o
oline
ocont
0
20406080
100
0cum
ulat
ive
F line [%
] Fline
= 1.44E-19 W/m2
1 10 100r [AU]
0.00.20.40.60.81.01.2
z/r
-6 -4 -2 0 2 4 6 8log n
CO [cm-3]
CO 4.844µm
10-810-610-410-2100102
o
oline
ocont
0
20406080
100
0cum
ulat
ive
F line [%
] Fline
= 1.15E-17 W/m2
0.1 1.0 10.0 100.0r [AU]
0.00.2
0.4
0.6
0.8
1.0
z/r
-6 -4 -2 0 2 4 6log n
CO [cm-3]
CO 4.844µm
10-810-610-410-2100102
o
oline
ocont
0
20406080
100
0cum
ulat
ive
F line [%
] Fline
= 1.46E-17 W/m2
0.1 1.0 10.0 100.0r [AU]
0.00.2
0.4
0.6
0.8
1.0
z/r
-6 -4 -2 0 2 4 6 8log n
CO [cm-3]
CO 4.844µm
10-610-410-2100102104
o
oline
ocont
0
20406080
100
0cum
ulat
ive
F line [%
] Fline
= 2.81E-17 W/m2
1 10 100r [AU]
0.00.20.40.60.81.01.2
z/r
-6 -4 -2 0 2 4 6 8log n
CO [cm-3]
Fig. 1.
7
[OI] 63μm
A. Carmona et al.: Understanding the circumstellar disk of HD135344B by multiwavelength observations and modeling
Model 33 Model 34 Model 46
[OI] 63.18µm
10-810-610-410-2100102
o
oline
ocont
0
20406080
100
0cum
ulat
ive
F line [%
] Fline
= 6.58E-17 W/m2
0.1 1.0 10.0 100.0r [AU]
0.00.2
0.4
0.6
0.8
1.0
z/r
0 2 4 6 8log n
O [cm-3]
[OI] 63.18µm
10-810-610-410-2100102
o
oline
ocont
0
20406080
100
0cum
ulat
ive
F line [%
] Fline
= 6.76E-17 W/m2
0.1 1.0 10.0 100.0r [AU]
0.00.2
0.4
0.6
0.8
1.0
z/r
0 2 4 6 8log n
O [cm-3]
[OI] 63.18µm
10-810-610-410-2100102
o
oline
ocont
0
20406080
100
0cum
ulat
ive
F line [%
] Fline
= 4.47E-17 W/m2
1 10 100r [AU]
0.00.20.40.60.81.01.2
z/r
0 2 4 6 8log n
O [cm-3]
CO 866.96µm
10-610-410-2100102104
o
oline
ocont
0
20406080
100
0cum
ulat
ive
F line [%
] Fline
= 1.32E-19 W/m2
0.1 1.0 10.0 100.0r [AU]
0.00.2
0.4
0.6
0.8
1.0
z/r
-6 -4 -2 0 2 4 6log n
CO [cm-3]
CO 866.96µm
10-610-410-2100102104
o
oline
ocont
0
20406080
100
0cum
ulat
ive
F line [%
] Fline
= 1.33E-19 W/m2
0.1 1.0 10.0 100.0r [AU]
0.00.2
0.4
0.6
0.8
1.0
z/r
-6 -4 -2 0 2 4 6 8log n
CO [cm-3]
CO 866.96µm
10-610-410-2100102104
o
oline
ocont
0
20406080
100
0cum
ulat
ive
F line [%
] Fline
= 1.44E-19 W/m2
1 10 100r [AU]
0.00.20.40.60.81.01.2
z/r
-6 -4 -2 0 2 4 6 8log n
CO [cm-3]
CO 4.844µm
10-810-610-410-2100102
o
oline
ocont
0
20406080
100
0cum
ulat
ive
F line [%
] Fline
= 1.15E-17 W/m2
0.1 1.0 10.0 100.0r [AU]
0.00.2
0.4
0.6
0.8
1.0
z/r
-6 -4 -2 0 2 4 6log n
CO [cm-3]
CO 4.844µm
10-810-610-410-2100102
o
oline
ocont
0
20406080
100
0cum
ulat
ive
F line [%
] Fline
= 1.46E-17 W/m2
0.1 1.0 10.0 100.0r [AU]
0.00.2
0.4
0.6
0.8
1.0
z/r
-6 -4 -2 0 2 4 6 8log n
CO [cm-3]
CO 4.844µm
10-610-410-2100102104
o
oline
ocont
0
20406080
100
0cum
ulat
ive
F line [%
] Fline
= 2.81E-17 W/m2
1 10 100r [AU]
0.00.20.40.60.81.01.2
z/r
-6 -4 -2 0 2 4 6 8log n
CO [cm-3]
Fig. 1.
5
SED
MCFOST ⟷ PRODIMO★ Goal: employ multi-instrument observations of gas and
dust of HD 135344B and constrain its disk structure.
★ Present status: found a model with similar SED, PAH spectrum, and line fluxes for the CO 4.7μm, [OI] 63 μm, and CO 866 μm emission.
★ To be included: near-IR interferometry, imaging, fit to the line profiles and other molecules detected.
CO 866 μm
CO 4.7μm
AU AU
AU
disk + high vel. outflow
Herschel 2012 Symposium C. Dougados.
SINFONI/VLT observations of the DG Tauri microjet
Receding jet
Approaching
jet
Star position
Background colors and red contours: [Fe II] atomic flow
Yellow contours: H2 1-0 S(1) emission
★ Continuum
Agra-Amboage, Dougados, Cabrit et al 2011!
Agra-Amboage, Cabrit, Dougados in prep.!
Dusty atomic flow
Slow molecular cavity
50 AU
PLANET'GAPS'IN'THE'DUST'LAYER'OF'3D'PROTOPLANETARY'DISKS'OBSERVABILITY,WITH,ALMA,
ALMA'SIMULATED'IMAGES'HYDRODYNAMIC'SIMULATIONS'OF'PLANET'GAPS'IN'DUSTY'DISKS''
Jean4François,Gonzalez1,,,Christophe,Pinte2,,,Sarah,Maddison3,,,François,Ménard2,,Laure,Fouchet4,,
MCFOST'+'
CASA'
350'µm
'85
0'µm
'1.3'mm'
TW HyaA dry desert or a steam bath?
What do the different Herschel lines tell us?
=> one model can still fit all line fluxes within a factor two=> need for multi-λ studies to unravel the full gas+dust disk structure=> HCO+ and [FeII] require very gas phase metal abundances below ISM value
I.Kamp, W.-F.Thi, G.Meeus, P.Woitke, I.Pascucci, B.Dent
Basic model from Thi et al. 2010, updated reaction rates, H2O surface chemistry
[Hogerheijde et al. 2012]
PACSPACS
Spitz
er
HIFI
steam bath inside 4 AU?
H2O ro-vib & rotational lines
Observa(ons+and+images+of+Young+Stellar+Objects+at+the+milli9arcsecond+scale:+the+case+of+MWC158+
J.#Kluska,#F.#Malbet,#J.0P.#Berger,#M.#Benisty,#B.#Lazareff,#J.0B.#Lebouquin#Young#Stellar#Objects#&#Milli0arcescond#Imaging##Problem#:##Strong#spectral#dependance#!##Three+methods+are+presented+:+
3. Parametric#fit#1. Removing#the#stellar#contribuOon#
2. Using#the#wavelengths#separately#
λ#
Rapid growth of gas-giant cores
by pebble accretion
Michiel Lambrechts & Anders JohansenLund Observatory
tg ⇡ td ⇡ ⌦�1K
+
�tH ⇡ 4⇥ 104⇣ r
5AU
⌘yr ⌧ 106...7 yr
Few stars in Upper Scorpius have sufficient disk massto form new giant planets
Geoff Mathews and the GASPS team
Mdust estimated from 1.2 and 1.3 mm photometry (Mathews et al. 2012). Mgas estimated by
comparison of gas line fluxes to mean gas masses from the DENT grid (e.g. Woitke et al. 2010,
Kamp et al. 2011).
Stellar-mass-independent disk structure
settling
mixing
Thank you!
