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The chemistry and stability of the protoplanetary disk surface

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

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The chemistry and stability of the protoplanetary disk surface

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  1. 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

  2. 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

  3. Motivation ? Protoplanetary disk in Orion Debris disk

  4. The basic model - 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

  5. Vertical density structure in a flaring T Tauri disk z/r [Dullemond et al. 2002] log UV radiation field of a T Tauri star scaled solar chromosphere + IUE data + stellar atmosphere model CO, H2 photodissociation [Kamp & Sammar 2004]

  6. The chemical structure -8 Interface disk-remnant gas -4 0 t= 1 layer H2 is chemically destroyed by O in the hot regions H2 + O  OH + H OH + n  O + H 500 K 2000 K

  7. The chemical structure Interface disk-remnant gas t= 1 layer • 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

  8. The gas temperature 500 K 50 K 2000 K 100 K Gas and dust couple well above the superheated surface layer of the disk

  9. The gas temperature  Gas and dust couple well above the superheated surface layer of the disk

  10. Evaporation 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

  11. Outlook: 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

  12. Outlook: 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

  13. Outlook: 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

  14. The End

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