I will present simulations of three-dimensional, magnetohydrodynamic accretion disks in the Kerr metric for a range of black hole spins and disk thicknesses.
These results illustrate that under the equilibrium conditions presented the DSE can accommodate dimensional and structure accretion changes from a random coil to a premolten globule without substantively populating the native state.
In three-dimensional simulations, the accretion rate may be obtained by measuring the spherically averaged density and velocity profiles (Abel et al. 2002; Yoshida et al. 2006; Gao et al. 2007; O'Shea and Norman 2007; Turk et al. 2011).
Siegel, D. M. & Metzger, B. D. Three-dimensional general-relativistic magnetohydrodynamic simulations of remnant accretion disks from neutron star mergers: outflows and r-process nucleosynthesis.
We carried out two dimensional high-resolution magnetohydrodynamic (MHD) simulations of an accretion disk around a weakly magnetized neutron star.
Jiang, Y.-F. Y.-F., Stone. & Davis, S. W. A global three-dimensional radiation magneto-hydrodynamic simulation of super-eddington accretion disks.
While analytical one-dimensional models have been enormously useful for understanding several aspects of accretion physics, other aspects such as the formation of jets and winds are beyond the scope of such models.
These instantaneous accretion rates generally agree with the power laws found in one-dimensional calculations.
Compared with traditional 3D geological models, the reservoir architecture model not only reflects complex sand body distribution in three-dimensional space but also indicates spatial distribution characteristics of inner architecture elements, such as the lateral accretion muddy layer inside the point bar.
Open image in new window Fig. 9 Establishment of 3D lateral accretion surface model combined with well data Open image in new window Fig. 10 Three-dimensional grid chart of architecture model in Ng33 thin layer Open image in new window Fig. 11 a Section map of architecture model in Ng33 thin layer.
Previous works using simplified neutrino treatments have shown that the evolution of accretion shock front formed during a CCSN differs significantly when axial symmetry is imposed, relative to full three dimensional simulations with no symmetries imposed.
