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Modeling the structure, chemistry and appearance of protoplanetary disks. Ringberg, Germany, april 2004. Disk structure and SEDs Dust properties Planet formation Disk/planet interaction Hydrodynamics. Transport processes Evaporation Gas physics Observations And many more…. Many topics.
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Modeling the structure, chemistry and appearance of protoplanetary disks Ringberg, Germany, april 2004
Disk structure and SEDs Dust properties Planet formation Disk/planet interaction Hydrodynamics Transport processes Evaporation Gas physics Observations And many more… Many topics
PDRs in disks • Advantages: • Seek comfort and security in the big cozy PDR community • Disk surfaces resemble PDRs • Well understood physics and chemistry
PDRs in disks • Drawbacks: • PDRs are 1-D, disks 2-D • How well do disks resemble the ISM? • Turbulent mixing • Dust physics
Dust in disks • There are NOfluffy grains! (C. Dominik) • They are porous (ma3) • Or fractal (mad, d<3) • Grain growth is slow, sometimes too slow • Electrostatic forces between charged grains can speed up the process • Aerodynamics may prevent shattering of porous grains
Dust evolution • How does the disk evolve observationally? • Amorphous → crystalline, or • Crystalline → amorphous • More processing in inner disk • Radial mixing can be very efficient
Mixing • Exact mechanism unknown; possible candidates are: • Magneto-rotational instability • Self gravity (only in very massive disks) • Baroclinic instability (Hubert Klahr) • Direction of radial mixing is uncertain (in near the midplane, out at the surface or vice versa?)
More mixing • Both radial and vertical mixing are very important for the chemistry • Hydro people: α-description incorrect to describe turbulence, mixing • Worse: angular momentum transfer α ≠ turbulent mixing α • What to do?
That’s (not quite) all • See http://www.mpia.de/PSF/WorkshopRingbergApril04 for workshop summary and ppt files