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MHD plus self-gravity for the dust, including particle feed back on the gas: gas dust Poisson equation solved via FFT in parallel mode: up to 256 3 cells 12/13/2009 Hubert Klahr - Planet Formation - MPIA Heidelberg Wednesday, September 5, 12
Formation Of Planetesimals From pressure trapped / gravitational Bound heaps of gravel - here magnetic turbulence: Johansen, Klahr & Henning 2011. Next: Raettig & Lyra 512 ^2 simulation 64 Mio particles Entire project used 15 Mio. CPU hours. 12/13/2009 Hubert Klahr - Planet Formation - MPIA Heidelberg Wednesday, September 5, 12 Concentration in Zonal Flows: 8
Page 1 and 2: The Role of Turbulence in Planetesi
Page 3 and 4: Turbulence in a non rotating frame:
Page 5 and 6: V e r t i c a l From dust/gas eq. 1
Page 7: Disk: 12/13/2009 Hubert Klahr - Pla
Page 11 and 12: Not the process but numerical resol
Page 13 and 14: Natalia Dziurkevich (in prep.) see
Page 15 and 16: 12/13/2009 Hubert Klahr - Planet Fo
Page 17 and 18: Ri 0.001 0.000 �0.001 �0.002
Page 19 and 20: 12/13/2009 Hubert Klahr - Planet Fo
Page 21 and 22: 2D axissymetric Pluto Simulation: T
Page 23 and 24: 2D axissymetric Pluto Simulation: R
Page 25 and 26: Interface MRI - Dead Zone linear ax
Page 27 and 28: Small particles in pressure maxima
Page 29 and 30: St = 0.05 particles (few millimeter
Page 31: Conclusions: Johansen and Klahr: Hi

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