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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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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

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

Motivation

?

Protoplanetary disk in Orion

Debris disk


The chemistry and stability of the protoplanetary disk surface

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


The chemistry and stability of the protoplanetary disk surface

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]


The chemistry and stability of the protoplanetary disk surface

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


The chemistry and stability of the protoplanetary disk surface

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


The chemistry and stability of the protoplanetary disk surface

The gas temperature

500 K

50 K

2000 K

100 K

Gas and dust couple well above

the superheated surface layer

of the disk


The chemistry and stability of the protoplanetary disk surface

The gas temperature

Gas and dust couple well above

the superheated surface layer

of the disk


The chemistry and stability of the protoplanetary disk surface

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


The chemistry and stability of the protoplanetary disk surface

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


The chemistry and stability of the protoplanetary disk surface

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


The chemistry and stability of the protoplanetary disk surface

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


The chemistry and stability of the protoplanetary disk surface

The End


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