thomas henning and dima semenov chemistry and dynamics in protoplanetary disks max-planck-institut...
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![Page 1: Thomas Henning and Dima Semenov Chemistry and Dynamics in Protoplanetary Disks Max-Planck-Institut für Astronomie, Heidelberg Courtesy of David E. Trilling](https://reader036.vdocuments.site/reader036/viewer/2022081518/5517a41855034645368b5bd7/html5/thumbnails/1.jpg)
Thomas Henning and Dima Semenov
Chemistry and Dynamics in Protoplanetary Disks
Max-Planck-Institut für Astronomie, Heidelberg
Courtesy of David E. Trilling
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Motivation
Initial conditions for planet formation
Chemical composition of primitive bodies in the solar system
Gas depletion and dissipation in disks – Molecules as tracers of disk history
Chemistry – Physical state of the disk (temperature, density, radiation, ionization, transport)
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Any Hot Topics?
Coupling between dynamics and chemistry
Complete evolutionary track from cold cores to
disks (e.g. deuteration sequence)
Coupling between solid-phase and gas-phase disk
components (grain evolution and settling)
Early stellar activity (winds, X-rays, UV, …)
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Disk Structure
~500 AU100 AU1 AU
~1000 AU
0
Observable region with interferometers
wind
photon-dominated layer
cold midplanewarm mol. layer
accretion (magneto-rotational instability)
hν, UV, X-rays
turbulent mixing
IS UV, cosmic rays
snowline
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Disk Physics
-7 ° - 7 ° (#20)ΩK = 12
Flux limited RT
3.5 - 6.5 AU (#51)
Highly Dynamical Environment
Klahr, Henning, and Kley (1999)
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N. Dziourkevitch & H. Klahr (2006), ApJ, in prep.
MRI OverviewR
otat
iona
l axi
s
Mag
neti
c fi
eld
geom
etry
faster rotation slower rotation
centrifugal force & magnetic tension loop generation(turbulence)
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Ionization Structure of a Disk: Effect of Grain Evolution
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Semenov, Wiebe, Henning (2004)
„Layered“ vertical structure
Ionization Structure of a Disk: Effect of Grain Evolution
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N2H+ in disks: CID Collaboration (Bordeaux – Heidelberg – Jena – Grenoble - Paris)
N2H+/HCO+ ~ 0.03
HCO+ is dominant ionN2H+ is not a good
tracer of ionization
Dutrey, Henning et al. (2006), A&A, submitted
10
1010
1012
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Dynamics and Chemistry
Chemically reacting flow system
„Well-mixed reactor system“
Flow along predominant direction including mixing
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Observational Evidence
Non-thermal line broadening (~100 m/s)
Crystalline silicates in comets and disks (van Boekel et al. 2005, Crovisier et al. 1997, Wooden et al. 2005)
Chondritic refractory inclusions in meteorites (MacPherson et al. 1988)
Gas-phase CO at T<25K in DM Tau (Dartois et al. 2003)
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Steady Inner Disk Model
no vertical mixing vertical mixing
CS CS
Ilgner, Henning et al. (2004)
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Previous Studies Gail & Tscharnuter (>2000): 2D hydro + RT inner disk,
gas-phase combustion chemistry, grain evolution crystalline silicate distribution, carbon chains
Ilgner et al. (2004; 2006a,b): 1+1D inner disk, 1D vertical mixing & radial transport, gas-grain chemistry molecular abundances
Lyons & Young (2005): inner solar nebula, 1D vertical mixing, photochemistry 16/18 oxygen isotopic anomalies
Willacy et al. (2006): 1+1D outer disk, 1D vertical chemistry, gas-grain + surface chemistry molecular abundances
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Chemistry with Dynamics
Input: Physical conditions, diffusion coefficient & flow data
Initial abundances of species A chemical network A numerical solver Benchmarking
iil
lliikj
kjjki UnnnDnnknnnk
t
n
H2H2
,
/
Evolution = Formation - Destruction + Diffusion - Advection [ Chemistry ] [ Dynamics ]
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Chemistry with Mixing
2D-implicit scheme for chemistry with mixing Fickian diffusion Full/reduced chemical networks1D-benchmarking with K. Willacy & D. Wiebe
Semenov , Wiebe, & Henning (2006), ApJL, submitted
t ~ N3 (amount of species in the model)
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Disk Model
1+1D flared disk (D‘Alessio et al. 1999) Mdisk= 0.05M, Mdot = 10-8M/yr, M = 0.65M, R >10 AU
Mixing efficiency D ~ 0.01csH (Johansen & Klahr 2005)
Radial D = 1.5 x vertical D ~ 1015 – 1018 cm2/g
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Overview of Mixing Results
10 AU 800 AU
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Disk Ionization Degree
Unaffected by diffusion since chemical equilibrium is reached quickly
Comp. Time: 2h 48h 24h >200h
Stationary Vertical mix. Radial mix. 2D-Mixing
30x65 grid, 200 species in 1600 reactions10 AU 800 AU
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Gas-phase CO at T<25K
Abundant CO gas in cold midplane despite fast freeze-out (steep local abundance gradients)
Stationary Vertical mix. Radial mix. 2D-Mixing
10 AU 800 AU
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N(CO) ~ 1017 cm-2 (2D-model) optical depth is ~ 1 explains the observations of Dartois et al. (2003)
Gas-phase CO at T<25K
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Gas-phase H2CO
Diffusion-dependent H2CO enrichment due to slow surface processes
100x lower diffusion
Stationary Vertical Radial 2D-Mixing
10x lower diffusion
10 AU 800 AU
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Basic Results
“Sandwich”-like disk structure is preserved
Ionization degree is hardly affected
Abundance of photo-controlled species are not affected
Abundances of more complex (organic) species can be enhanced (grain mantle components, e.g.
H2CO)
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Disk Chemistry
Large range of temperatures and densities
Importance of radiation fields
Strong coupling between chemistry and dynamics (ionization, temperature structure, …)
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Collaborators
CID collaboration (A. Dutrey, S. Guilloteau, V. Pietu, A. Bacmann, R. Launhardt, Y. Pavlyuchenko, J. Pety, K. Schreyer, V. Wakelam)
D. Wiebe (Moscow): Chemistry with mixing
M. Ilgner (London): Chemistry with mixing
H. Klahr, A. Johansen (MPIA): Disk dynamics
K. Dullemond (MPIA): Grain evolution
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The End