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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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Presentation Transcript
slide1

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

slide2

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

slide3

Motivation

?

Protoplanetary disk in Orion

Debris disk

slide4

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

slide5

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]

slide6

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

slide7

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

slide8

The gas temperature

500 K

50 K

2000 K

100 K

Gas and dust couple well above

the superheated surface layer

of the disk

slide9

The gas temperature

Gas and dust couple well above

the superheated surface layer

of the disk

slide10

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

slide11

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

slide12

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

slide13

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

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