blue dots workshop in paris, nov 17/18, 2008 key questions in planet formation and evolution

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Blue Dots Workshop in Paris, Nov 17/18, 2008 Key Questions in Planet Formation and Evolution Hans Zinnecker (AIP, Potsdam) Sebastian Wolf (Univ. Kiel) 1. core accretion vs. grav. instability 2. planet formation in single vs. binary systems 3. circumstellar disk evolution and planet formation as a function of host mass and metallicity 4. circumstellar disk evolution and planet formation as a function of environment: low-mass vs. high-mass star forming regions 5. are giant outer planets a prerequisite for inner telluric planets with habitable zones? 6. is the architecture of the solar system unique? PS. moons around planets, planetary magnetic fields? galactic habitable zones: bulge, disk, halo, clusters? free-floating earth-mass planets (ejected systems)? How can we attack these questions observationally? Which are the most relevant observable parameters?

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Blue Dots Workshop in Paris, Nov 17/18, 2008 Key Questions in Planet Formation and Evolution Hans Zinnecker (AIP, Potsdam) Sebastian Wolf (Univ. Kiel) 1.core accretion vs. grav. instability 2. planet formation in single vs. binary systems - PowerPoint PPT Presentation

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Page 1: Blue Dots Workshop in Paris, Nov 17/18, 2008 Key Questions in Planet Formation and Evolution

Blue Dots Workshop in Paris, Nov 17/18, 2008

Key Questions in Planet Formation and Evolution

Hans Zinnecker (AIP, Potsdam)Sebastian Wolf (Univ. Kiel)

1. core accretion vs. grav. instability2. planet formation in single vs. binary systems3. circumstellar disk evolution and planet formation as a function of host mass and metallicity4. circumstellar disk evolution and planet formation as a function of environment:

low-mass vs. high-mass star forming regions5. are giant outer planets a prerequisite for inner telluric planets with habitable zones?6. is the architecture of the solar system unique?

PS. moons around planets, planetary magnetic fields? galactic habitable zones: bulge, disk, halo, clusters?

free-floating earth-mass planets (ejected systems)?

How can we attack these questions observationally?Which are the most relevant observable parameters?

Page 2: Blue Dots Workshop in Paris, Nov 17/18, 2008 Key Questions in Planet Formation and Evolution

Blue Dots "Planet Formation" Team:

H. Zinnecker (chair) [email protected]. Wolf (co-chair) [email protected]

Y. Alibert (Bern) [email protected]. Benz (Bern) [email protected]. Blum (Braunschweig) [email protected]. Dullemond (Heidelberg) [email protected]. Dutrey (Bordeaux) [email protected]. Johansen (Leiden) [email protected]. Klahr (Heidelberg) [email protected]. Kley (Tübingen) [email protected]. Krivov (Jena) [email protected]. Meyer (Zürich)? [email protected]

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Left: Density structure after 200 Orbits. Red high density, blue low density.

Right: Flow field in the vicinity of the planet. In green the Roche lobe.

credit: W. Kley

Page 19: Blue Dots Workshop in Paris, Nov 17/18, 2008 Key Questions in Planet Formation and Evolution

Left: Density structure after 1400 yrs.High resolution calculation with inner disk.Parameter for HD 73526, m1=2.9 MJup, m2=2.5 MJup.

Right: Semi-major axis and eccentricity evolution.Capture in 2:1 mean-motion-resonance occurs at t=400 yrs.

credit: W. Kley

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Kalas et al. 2008

HST observations

Page 33: Blue Dots Workshop in Paris, Nov 17/18, 2008 Key Questions in Planet Formation and Evolution

Marois et al. 2008

Keck/Gemini-N observations

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