MHD Turbulence Under the Virtual Microscope Gregory L. Eyink - - PowerPoint PPT Presentation
MHD Turbulence Under the Virtual Microscope Gregory L. Eyink Applied Mathematics & Statistics and Physics & Astronomy The Johns Hopkins University 8th International Conference on Numerical Modeling of Space Plasma Flows July 1st -
The Astrophysical Journal, 769:156 (20pp), 2013 June 1 Schnittman, Krolik, & Noble Figure 2. Fluid density profile for a slice of Harm3d data in the (r, z) plane at simulation time t = 12,500M. Contours show surfaces of constant optical depth with τ = 0.01, 0.1, 1.0. Fiducial values for the black hole mass M = 10 M and accretion rate ˙ m = 0.1 were used. (A color version of this figure is available in the online journal.) Figure 3. Magnetic energy density profile for a slice of Harm3d data in the (r, z) plane corresponding to the same conditions as in Figure 2. (A color version of this figure is available in the online journal.)
The Astrophysical Journal, 769:156 (20pp), 2013 June 1 Schnittman, Krolik, & Noble Figure 2. Fluid density profile for a slice of Harm3d data in the (r, z) plane at simulation time t = 12,500M. Contours show surfaces of constant optical depth with τ = 0.01, 0.1, 1.0. Fiducial values for the black hole mass M = 10 M and accretion rate ˙ m = 0.1 were used. (A color version of this figure is available in the online journal.) Figure 3. Magnetic energy density profile for a slice of Harm3d data in the (r, z) plane corresponding to the same conditions as in Figure 2. (A color version of this figure is available in the online journal.)
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