Hubert KLAHR

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Magneto Rotational Instability (MRI) drives turbulence in accretion disks 12/13/2009 <strong>Hubert</strong> Klahr - Planet Formation - MPIA 14 Simulation by Mario Heidelberg Flock using the Pluto code.
Pluto Code: HLLD Upwind CT, piecewise linear reconstruction, Runge Kutta 2nd order 384x192x768 Flock, Dzyurkevich, Klahr, Turner, Henning, 2011 12/13/2009 <strong>Hubert</strong> Klahr - Planet Formation - MPIA Heidelberg Global 360 stratified! At 20 grid cells per H! 15 1.8 Million CPU hours
Page 1 and 2: Les Houches, Feb. 7 th , 2013 Disk
Page 3 and 4: Outline: The role of Turbulence in
Page 5 and 6: Planet Formation time Surface stick
Page 7 and 8: Laminar disk: No growth beyond 10cm
Page 9 and 10: What if there is no global turbulen
Page 11 and 12: 10 cm sized boulders: V e r t i c a
Page 13: Turbulence in Disks: Candidates •
Page 17 and 18: Development of MHD Turbulence From
Page 19 and 20: 2,000,000 boulders of 1m size 12/13
Page 21 and 22: MHD plus self-gravity for the dust,
Page 23 and 24: 14 years back... ...before I was do
Page 25 and 26: 3D - Radiation Hydro of Convection
Page 27 and 28: Vorticity Vorticity: Pencil Code: L
Page 29 and 30: 2D - vertically integrated disk (Kl
Page 35 and 36: Density: zimuthal 12/13/2009 Hubert
Page 37 and 38: 12/13/2009 Hubert Klahr - Planet Fo
Page 39 and 40: Klahr & Raettig in prep. Using data
Page 41 and 42: Richardson number & N 2 = thermal d
Page 43 and 44: Pluto Code: 1024^2; WENO3-RK3; HLLE
Page 45 and 46: 2D Local (radial - vertical), Inclu
Page 47 and 48: 2D axissymetric Pluto Simulation: O
Page 49 and 50: 12/13/2009 Hubert Klahr - Planet Fo
Page 51 and 52: Full 3D Pluto Simulation: Spontanou
Page 53 and 54: Vertical Buoyancy Frequency: Includ
Page 55 and 56: Interface MRI - Dead Zone Disk Weat
Page 57 and 58: St = 0.05 particles (few millimeter

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