the chemistry and stability of the protoplanetary disk surface
DESCRIPTION
The chemistry and stability of the protoplanetary disk surface. Inga Kamp In collaboration with: Kees Dullemond (MPA) Ewine van Dishoeck (Leiden) Bastiaan Jonkheid (Leiden). David Hardy, NASA. The chemistry and stability of the protoplanetary disk surface. Inga Kamp - PowerPoint PPT PresentationTRANSCRIPT
![Page 1: The chemistry and stability of the protoplanetary disk surface](https://reader035.vdocuments.mx/reader035/viewer/2022070401/568135d2550346895d9d3d1f/html5/thumbnails/1.jpg)
The chemistry and stability ofThe chemistry and stability ofthe protoplanetary disk surfacethe protoplanetary disk surface
Inga Kamp
In collaboration with:
Kees Dullemond (MPA)
Ewine van Dishoeck (Leiden)
Bastiaan Jonkheid (Leiden)
David Hardy, NASA
![Page 2: The chemistry and stability of the protoplanetary disk surface](https://reader035.vdocuments.mx/reader035/viewer/2022070401/568135d2550346895d9d3d1f/html5/thumbnails/2.jpg)
The chemistry and stability ofThe chemistry and stability ofthe protoplanetary disk surfacethe protoplanetary disk surface
Inga Kamp
In collaboration with:
Kees Dullemond (MPA)
Ewine van Dishoeck (Leiden)
Bastiaan Jonkheid (Leiden)
David Hardy, NASA
![Page 3: The chemistry and stability of the protoplanetary disk surface](https://reader035.vdocuments.mx/reader035/viewer/2022070401/568135d2550346895d9d3d1f/html5/thumbnails/3.jpg)
MotivationMotivation
??
Protoplanetary disk in Orion
Debris disk
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The basic modelThe basic model
density distribution
gas temperaturechemical composition
dust temperature
heating/coolingequilibrium
chemistry
- disk masses: 10-4 - 0.01 M Sun
- elemental abundances: molecular cloud abundances
- optical properties of dust grains: single 'mean' grain size
- dust temperature: radiative equilibrium
- gas-to-dust mass ratio: variable
- UV radiation fields: interstellar radiation field, photospheric radiation field, photosphere+chromosphere
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Vertical densitystructure in a flaring T Tauri disk
[Dullemond et al. 2002]
CO, H2 photodissociation
UV radiation field of a T Tauri star
scaled solar chromosphere + IUE data + stellar atmosphere model
[Kamp & Sammar 2004]
log
z/r
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The chemical structureThe chemical structure
= 1 layer
Interface disk-remnant gas
2000 K
500 K
-4
0
-8
H2 is chemically
destroyed by O inthe hot regions
H2 + O OH + HOH + O + H
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The chemical structureThe chemical structure
= 1 layer
Interface disk-remnant gas
- warm H2 present in disk surface
layers (thermally excited, Tex~ few 100 K)
- warm surface contains observable molecules such as e.g. CO, CH, OH
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The gas temperatureThe gas temperature
Gas and dust couple well abovethe superheated surface layerof the disk
2000 K
500 K
100 K
50 K
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The gas temperatureThe gas temperature
Gas and dust couple well abovethe superheated surface layerof the disk
![Page 10: The chemistry and stability of the protoplanetary disk surface](https://reader035.vdocuments.mx/reader035/viewer/2022070401/568135d2550346895d9d3d1f/html5/thumbnails/10.jpg)
Evaporation of the surfaceEvaporation of the surface
- Gas densities are high enough to couple H to the remaining species
- Disk surface evaporates inside of ~50 AU verify with fully self-consistent disk models
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Structure of the diskfrom the assumption of
hydrostatic equilibrium
Chemistry
Gastemperature
Outlook: Disk structure modelsOutlook: Disk structure models
- self-consistent stationary disk models
- comparison with observations by scanning through the disk with e.g. VISIR, IRAM, ALMA in the NIR to submm feedback for the models
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Structure of the diskfrom the assumption of
hydrostatic equilibrium
Chemistry
Gastemperature
Outlook: Disk structure modelsOutlook: Disk structure models
- self-consistent stationary disk models
- comparison with observations by scanning through the disk with e.g. VISIR, IRAM, ALMA in the NIR to submm feedback for the models
![Page 13: The chemistry and stability of the protoplanetary disk surface](https://reader035.vdocuments.mx/reader035/viewer/2022070401/568135d2550346895d9d3d1f/html5/thumbnails/13.jpg)
Structure of the diskfrom the assumption of
hydrostatic equilibrium
Chemistry
Gastemperature
Outlook: Disk structure modelsOutlook: Disk structure models
- self-consistent stationary disk models
- comparison with observations by scanning through the disk with e.g. VISIR, IRAM, ALMA in the NIR to submm feedback for the models
- evaporation of the inner disk as a function of spectral-type of central star (include X-rays)
- compile heating/cooling tables for hydrodynamical modeling
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The EndThe End