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Because the magneto-rotational instability is capable of exponentiallyamplifying weak preexisting magnetic fields, it might be hoped that thecharacter of the magnetic field in accretion disks is independent of the natureof the seed field. However, the divergence-free nature of magnetic fields inhighly conducting fluids ensures that their large-scale topology is preserved,no matter how greatly the field intensity is changed. By performing globaltwo-dimensional and three-dimensional general relativistic magnetohydrodynamicdisk simulations with several different topologies for the initial magneticfield, we explore the degree to which the character of the flows around blackholes depends on the initial topology. We find that while the qualitativeproperties of the accretion flow are nearly independent of field topology,jet-launching is very sensitive to it: a sense of vertical field consistent forat least an inner disk inflow time is essential to the support of strong jets.

The Influence of Magnetic Field Geometry on the Evolution of Black Hole Accretion Flows: Similar Disks, Drastically Different Jets