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A Vorticity-preserving Hydrodynamical Scheme for Modeling Accretion Disk Flows

  • Authors: Darryl Seligman, and Gregory Laughlin

2017 The Astrophysical Journal 848 54.

  • Provider: AAS Journals

Caption: Figure 6.

Initial velocity profile of the vortex seeded into a Keplerian shear flow, evolved by the RBV2, PLUTO, and ZEUS algorithms for compressible flow, and depicted in Figure 7. The vortex profile is created following the prescription given by Adams & Watkins (1995). We use shearing box simulations (Hawley et al. 1995) with a radial and azimuthal extent of ﹩{\rm{\Delta }}R=0.04\,\mathrm{au}﹩ centered at R = 1 au with a sound speed cs = 0.050, such that the Mach number of the shear at the radial boundaries, ﹩v=\pm 0.029﹩, is ﹩{ \mathcal M }\approx 0.75﹩. The maximum vortex velocity, ﹩v=\pm 0.025﹩, is comparable to the maximum shear velocity, such that close to the fiducial radius the flow is dominated by the vortex. Note that the units on the x- and y-axes indicate the grid elements of the simulation.

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