structure and evolution of protoplanetary disks · variability of seds: ux orionis stars (uxors)...
TRANSCRIPT
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Structure and Evolution of Protoplanetary Disks
Review Talk
C.P. Dullemond Institute for Theoretical Astrophysics (ITA/ZAH)
Heidelberg, Germany
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This session as a word cloud:
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Made with: www.wordle.net
This session as a word cloud:
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Figure from: Dullemond & Monnier (2010) Ann. Rev. A&A
Main features of a protoplanetary disk
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Radial distribution of matter
Andrews et al. (2009)
SED + millimeter resolved maps (=visibility values)
VSSG 1
WSB 60
SED fitting mm-interferometry (visibility fitting)
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Radial distribution of matter
asteroids
Earth+Mars +Venus
Mercury Jupiter
Saturn
Uranus+ Neptune
Andrews et al. (2009)
See also poster 78 Wright
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Non-stationary (spreading) disks
Time steps of 2x105 year
Lynden-Bell & Pringle (1974), Hartmann et al. (1998)
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Evolution of disk parameters
(after Hueso & Guillot 2005)
Class O, I Class II
See also poster 47 Manara and poster 63 Ratzka on disk evolution
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However: disks are not axially symmetric...
Fukagawa et al. 2004
Scattered light
AB Aurigae
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However: disks are not axially symmetric...
Oppenheimer et al. 2008
Scattered light, polarized component
See also talk by Panic See poster 13 Demidova, poster 33 Juhasz, poster 65 Rosenfeld, poster 66 Ruge (?)
AB Aurigae
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Vertical structure of a protoplanetary disk
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Still one of the nicest disk images:
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Flaring disk structure: irradiation
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Creation of a warm surface layer
Calvet et al. 1991 Malbet & Bertout 1991 Chiang & Goldreich 1997
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T Tauri Star SEDs:
Spitzer IRS spectra of large sample of class II sources. Shown here: the sources with the flattest SEDs, i.e. strongest disk flaring.
Furlan et al. 2006
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Vertical temperature structure
Model from Paola D’Alessio (from: Dullemond, Hollenbach, Kamp & D’Alessio PPV review)
See poster 50 Mulders
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Cold midplane layers: Ice-coated dust?
(i.e. where is the „snow line“?)
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Davis (2005)
Where is the ‘snow line’?
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Where is the ‘snow line’?
Davis 2005 Lecar, Podolak, Sassalov & Chiang 2006
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Where is the ‘snow line’?
Davis 2005
Time [years]
R [A
U]
Davis 2005 Lecar, Podolak, Sassalov & Chiang 2006
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Where is the ‘snow line’?
10-7 a=0.01
0 2 4 6 8 10 12 14R [AU]
0.0
0.5
1.0
1.5
2.0
2.5
3.0
z [A
U]
Min, Dullemond, Dominik & Kama 2011
First fully 2-D/3-D radiative transfer model of snow line
dM/dt = 10-7 M¤/yr, α=0.01
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Where is the ‘snow line’?
10-8 a=0.01
0 1 2 3 4 5R [AU]
0.0
0.2
0.4
0.6
0.8
1.0
z [A
U]
dM/dt = 10-8 M¤/yr, α=0.01
First fully 2-D/3-D radiative transfer model of snow line
Min, Dullemond, Dominik & Kama 2011
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Where is the ‘snow line’?
10-9 a=0.01
0.0 0.5 1.0 1.5 2.0R [AU]
0.0
0.1
0.2
0.3
0.4
z [A
U]
dM/dt = 10-9 M¤/yr, α=0.01
First fully 2-D/3-D radiative transfer model of snow line
Min, Dullemond, Dominik & Kama 2011 See talk Dominik, See poster 31 Honda poster 73 Terada
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Warm surface layers: rich in molecules?
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Warm surface layers: rich in molecules?
Model from Paola D’Alessio (from: Dullemond, Hollenbach, Kamp & D’Alessio PPV review)
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See talk Dominik about theoretical interpretation See talk Hogerheijde about the latest on H2O in disks More on molecules in disks: see talks by Mandell and by Banzatti, see poster 43 Lahuis
The dryness of the surface layers
Several disks have much weaker H2O vapor lines in their Herschel spectra than expected from models. Conclusion: Their outer disk surface layers appear to be „dry“. Bergin, Hogerheijde et al. 2010
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Vertical temperature structure The very upper layers
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Vertical temperature structure The very upper layers
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Vertical temperature structure The very upper layers
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Vertical temperature structure The very upper layers
Gorti & Hollenbach 2008
For atomic line emission from these regions: Talks by Rigliaco and by Sacco
For thermally driven outflow (i.e. disk photoevaporation) see talks by Alexander and by Owen
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The evolution of the dust population
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How is dust ‘size’ measured? Example: Opacity of spherical silicate
grain at various sizes
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So... What is observed?
R. van Boekel et al. (2003), A&A 400L, 21
Small grains
Big grains
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Dust coagulation model with fragmentation
10-8
10-6
10-4
10-2 Σ d
ust [
g/cm
2 ]
Grain size [cm] 10-4 10-2 100
Birnstiel, Dullemond & Ormel 2010
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Measuring grain sizes from mm obs
Ricci, Testi, Natta, Neri, Cabrit & Herczeg (2010)
See talks by Ricci, by Testi and by Carpenter See poster 9 by Ubach Catarina
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Comparing model to observation
Data: Isella et al. 2010 Model: Birnstiel, Ricci, Trotti et al. 2010
Data for large sample
Model prediction
Radial dependence in the disk?
smaller grains in outer disk
larger grains in inner disk
β
See talks by Ricci and by Birnstiel
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Essential for dust growth: Turbulence and vortices
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Standard model for turbulence: MRI
Flock et al. 2011; Dzyurkevich et al. 2010 for global MRI models
See poster Mario Flock Observ. constraning turbulence: Talk by Simons
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But: there is a „dead zone“ Gammie 1996 Here: Turner & Sano 2008
See talk by Ilgner on grains & electric charge, See poster 2 Ataiee, poster 16 Dzyurkevich, poster 18 Faure
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Vortices in protoplanetary disks
Vortex generation by baroclinic instability (Klahr & Bodenheimer 2003)
Raettig (PhD thesis 2012)
See poster 48 Meheut on Rossby vortices
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Vortices as particle traps
Barge & Sommeria 1995; Klahr & Henning 1997 Here from: Raettig (PhD thesis 2012)
More on particle traps: See talk Pinilla
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Non-steady phenomena in protoplanetary disks
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Episodic accretion of gas onto the disk M
[M¤ /yr]
10-7
10-6
10-5
10-4
10-3
0.0
-0.5
0.5
1.0
1.5
j [10
20 c
m2 /s
M
j
0.0 0.5 1.0 1.5
2.0
t [Million years]
Jappsen & Klessen 2004
Result from model of turbulent star formation
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Episodic accretion of gas onto the disk AB Aurigae: Perhaps an example of a recently acquired disk?
Fukagawa et al. 2004 Pietu, Guilloteau & Dutrey 2005 See also Corder et al. 2005
Spiral structures Off-center mm disk
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Episodic accretion of gas onto the disk AB Aurigae: Perhaps an example of a recently acquired disk?
Evidence for small pristine dust from steep mm slope
Evidence for Inflow of gas from large distances
Grady et al.1999
See talk by I. Thies for models of episodically accreting disks
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Variable accretion in disks: FU Orionis stars
Model by Zhu et al. 2010
Variability time scale: 103..105 yr Possible origin: - Instability of the dead zone (Armitage, Livio & Pringle 2001), - possibly triggered by a massive planet (Lodato & Clarke 2004) - Gravitational instability of continuously fed disk (Vorobyov & Basu 2004)
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Thermal instability in the disk
€
Q+ <Q−€
Q+ >Q−€
Q+ <Q−T [K]
See poster 34 Keisuke (?), see poster 51 Müller on gravitational instability of irradiated disks
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Variable accretion in disks: EX Lupi stars (EXOrs)
Variability time scale: 0.1 .. 100 yr Possible origin: - Instability of the magnetic disk truncation point (D‘Angelo & Spruit 2010) - ??
EX Lupi outburst of 2008
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Variable accretion in disks: EX Lupi stars (EXOrs)
Abraham, Juhasz et al. Nature, 2009
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Variable accretion in disks: EX Lupi stars (EXOrs)
λ [µm]
Flux
Before outburst
λ [µm]
Flux
Amorphous dust
λ [µm]
Flux
During outburst
Abraham, Juhasz et al. Nature, 2009
Peaks indicative of crystalline dust
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Variable accretion in disks: EX Lupi stars (EXOrs)
Wobbling inner disk of EX Lupi:
Goto, Regaly et al. 2011
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Model for EXOr variability Unstable magnetic truncation point („X-point“)
D‘Angelo & Spruit 2010
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Model for EXOr variability Unstable magnetic truncation point („X-point“)
D‘Angelo & Spruit 2010
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Variability of SEDs: UX Orionis stars (UXOrs)
Pontoppidan et al. 2007
Example here: VV Serpens
Time scale: weeks Probable origin: - Dusty gas filaments passing through line of sight toward the star. Must be from very inner disk (time scale argument)
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Variability of SEDs: Pivoting SEDs
Muzerolle et al. 2009
Example here: LRLL 31
Time scale: months/yrs Probable origin: - Varying height of the inner dust rim (for some reason see talk by Turner) - Pivoting likely due to the corresponding variable shadowing
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Variability of SEDs: UX Orionis stars (UXOrs)
See talk by Neal Turner
Time scale: weeks Probable origin: - Dusty gas filaments passing through line of sight toward the star. Must be from very inner disk (time scale argument) - Pivoting likely due to the corresponding variable shadowing
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So now we have arrived at the very inner disk regions
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The inner disk regions
Figure from: Dullemond & Monnier (2010) Ann. Rev. A&A
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Rounded shape of dust rim
Originally shown by Isella & Natta 2005
Here: 2-D radiative transfer model by Kama et al. 2009 See also Tannirkulam et al. 2008
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But the real mystery lies closer in... The very inner disk appears to be inconsistent with molecular or
even atomic gas! Is there still some dust surviving there?
Benisty et al. 2010
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Disks with huge holes („Transition disks“)
Death of a disk
and/or birth of a planetary system
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“Transition disks”: Huge inner holes
D’Alessio et al. 2005, Forrest et al. 2004
CoKu Tau 4
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“Transition disks”: Huge inner holes
1 AU 40 AU
200AU
Normal disk
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“Transition disks”: Huge inner holes
Disk with inner cavity
1 AU 40 AU
200AU See talks by Alexander and by Owen See poster 38 Koepferl poster 49 Menu, poster 69 Salinas, poster 70 Sanz-Forcada
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Can the birth of a „solar system“ be the cause?
Zhu et al. 2011
Just the existence of planets does not seem to cause a strong enough „inner hole“ Need dust dynamics and growth (e.g. Rice et al.)
See talks by Andrews, by Birnstiel and by Pinilla
Observability of gaps: see talk by Gonzalez
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Transition disks: Ring-like structures
LkHa 330 SR 21 HD 135344B
Brown et al. 2009
See also talks by Schreiber and by Meru
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Asymmetries (if real): Dynamical origin? Observations: Model:
Regaly, Juhasz, Sandor et al. 2012 (Observations by Brown et al. 2009)
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When the gas is gone:
From planet(esimals) back to dust...
„Debris disks“
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Fomalhaut: a nearby debris disk
Kalas NASA/ESA
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Fomalhaut: a nearby debris disk
Acke, Min, Dominik et al. 2012
As seen by Herschel PACS @ 70 microns
See talks by Krivov and by Ertel See poster 14 Donaldson, poster 17 Faramaz, poster 22 Fujiwara poster 29 Harvey poster 40 Kral poster 45 van Lieshout poster 46 Loehne
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That‘s it for this overview...
Now let‘s hear what the speakers of this session have to say!