1. “The hot bubbles around nascent planets :
Stars to Disks
Gainesville - Apr. 14th 2007
“The hot bubbles around nascent planets :
Influence on migration, accretion and detectability”
Smaller objects but also
Hubert Klahr, MPI für Astronomie
Willy Kley, Tübingen & Sebastian Wolf, MPIA
Geoff Bryden, JPL; Kees Dullemond, Thomas Henning,
Oliver Fernandez, etc. MPIA; Doug Lin Santa Cruz
Hubert Klahr - Planet Formation - MPIA Heidelberg

2. Hubert Klahr - Planet Formation - MPIA Heidelberg
Outline: Motivation: Pop. Synthesis Klahr & Kley The hot blob -- photosphere Influence on migration rates Observability Conclusions/Outlook
Hubert Klahr - Planet Formation - MPIA Heidelberg

3. Hubert Klahr - Planet Formation - MPIA Heidelberg
Jupiter mass at 5AU
3D radiation hydro of planet disk interaction with the TRAMP code.
Van Leer Hydro plus flux limited diffusion at 100x200x25 grid cells:
domain: 1.25 AU < r < 25 AU
Hubert Klahr - Planet Formation - MPIA Heidelberg
Klahr & Feldt 2004; Klahr & Kley 2006

5. Hubert Klahr - Planet Formation - MPIA Heidelberg
Outline: Klahr & Kley Zoom down to the Jupiter surface! Two new cases: 9 & 30 Mearth The hot blob -- photosphere Influence on migration rates Conclusions/Outlook
Hubert Klahr - Planet Formation - MPIA Heidelberg

6. Population Synthesis: Extrasolar giant planet formation models
See also Poster P5-9 by Christophe Mordasini!
Courtesy: Willy Benz and the Bern group/see also Ida & Lin

7. Known Planets: Courtesy by Jeremy Richardson May 2006
Based on data compiled by J. Schneider

8. Hubert Klahr - Planet Formation - MPIA Heidelberg
Jupiter mass at 5AU
3D radiation hydro of planet disk interaction with the TRAMP code.
Van Leer Hydro plus flux limited diffusion at 100x200x25 grid cells:
domain: 1.25 AU < r < 25 AU
Hubert Klahr - Planet Formation - MPIA Heidelberg
Klahr & Feldt 2004; Klahr & Kley 2006

9. A Young Jupiter... > 1000yrs
Temperature, velocity and density contours.

10. Disk or Donut around Jupiter?
Bad times for Planets
Pressure scale height in “Blob” over the Roche lobe.

11. A Young Jupiter... > 1000yrs
Temperature, velocity and density contours.

12. Color = photospheric temp.
vs. photosph. Height of disk!
height
phi
radius

13. Hubert Klahr - Planet Formation - MPIA Heidelberg
High res.:
Color = photospheric temp.
Hubert Klahr - Planet Formation - MPIA Heidelberg

14. Color = photospheric temperature
Photospheric height.
high res.: 30 Mearth
Hubert Klahr - Planet Formation - MPIA Heidelberg

15. Color = temperature -- surface = height high res.: 9 Mearth
accretion & migration rates as function of: planet and disk mass, location, turbulence, opacity, irradiation, etc.
Hubert Klahr - Planet Formation - MPIA Heidelberg

16. Negative = outward drift! Caveat: is in a Dead Zone
Torques for a 9 MEarth planet:
Random migration or
Type XXXIX migration?
Shift in corotation torques
Negative = outward drift!
Caveat: is in a Dead Zone

17. Paardekooper & Mellema As well as our simulations
Warning:
Paardekooper & Mellema
As well as our simulations
Had no viscosity, e.g. dead zone.
Unpredictable disk evolution.
Remember talks by Matsumura and Pudritz
% planet-disk
% planet-disk % planet-disk
Outward drift: -10-4/yr
after D’Angelo, Henning & Kley 2003b plus new results by: Klahr, Bryden & Kley also found by Paardekooper & Mellema

18. Hubert Klahr - Planet Formation - MPIA Heidelberg
Dead zone evolution:
This is 2D... What happens in 3D?
Wünsch, Klahr & Rozyczka, 2005
Hubert Klahr - Planet Formation - MPIA Heidelberg

19. Inner Rim: with Kees Dullemond
Hydro + flux limited Diffusion + ray tracing
Inner Rim: with Kees Dullemond

20. Hubert Klahr - Planet Formation - MPIA Heidelberg
Height and temperature of photosphere for disk emission
in the case of irradiation from the central object:
Flux limited diffusion plus ray tracing during the hydro run!
Hubert Klahr - Planet Formation - MPIA Heidelberg

21. Scattered light and photosphere for irradiation:

22. Test of Radiation transport: scattered light/role of inner disk
TRAMP (Radiation- Hydro)
MC3D (S. Wolf)

23. Test of Radiation transport: scattered light
emitted light

24. Test of Radiation transport: scattered light
emitted light

25. Imaging in the Mid-infrared (~10micron)
Hot Accretion Region around the Planet
10mm surface brightness profile of a T Tauri disk with an embedded planet (inner 40AUx40AU, distance: 140pc)
[Wolf & Klahr 2005]
i=0deg
i=60deg
Science Case Study for T-OWL:
Thermal Infrared Camera for OWL (Lenzen et al. 2005)
Justification of the Observability in the Mid-IR for nearby objects (d<100pc)

26. Hubert Klahr - Planet Formation - MPIA Heidelberg
Conclusions:
migration depends on disk evolution. ;)
MHD/dead-zone/Irradiation/Evaporation/
multiple Planets/etc.
...thats why comparisons to upcoming instruments/observations are so important! (VLTI, LBT, ALMA, ELT etc. )
Embedded Planets will be our measuring device for accretion disk physics!
Hubert Klahr - Planet Formation - MPIA Heidelberg

27. Hubert Klahr - Planet Formation - MPIA Heidelberg
Outlook:
1.) Parameter Study: Disk Mass/position/Planet Mass
2.) => feeding Population Synthesis Simulations
3.) MPI version of TRAMP for “PIA” (256 processors)
Hubert Klahr - Planet Formation - MPIA Heidelberg

28. Temperature, velocity and density contours.
A Very Young Jupiter...

29. Transiting Planets: mass + radius
We need to learn how they migrate and stop there!