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This article reports on three-dimensional (3-D) MHD simulations ofnon-rotating and rapidly rotating black holes and the adjacent black holeaccretion disk magnetospheres. A particular emphasis is placed on the verticalmagnetic flux that is advected inward from large radii and threads theequatorial plane near the event horizon. In both cases of non-rotating androtating black holes, the existence of a significant vertical magnetic field inthis region is like a switch that creates powerful jets. There are manysimilarities in the vertical flux dynamics in these two cases in spite of thetremendous enhancement of azimuthal twisting of the field lines and enhancementof the jet power because of an "ergospheric disk" in the Kerr metric. A 3-Dapproach is essential because two-dimensional axisymmetric flows are incapableof revealing the nature of vertical flux near a black hole. Poloidal fieldlines from the ergospheric accretion region have been visualized in 3-D andmuch of the article is devoted to a formal classification of the differentmanifestations of vertical flux in the Kerr case.

Three Dimensional Simulations of Vertical Magnetic Flux in the Immediate Vicinity of Black Holes