Astronomy and Astrophysics – Astrophysics
Scientific paper
2007-09-24
Astronomy and Astrophysics
Astrophysics
42 pages; 17 figures; Accepted for publication in ApJ (some new discussion and 2 new figures)
Scientific paper
10.1086/533492
Because the magneto-rotational instability is capable of exponentially amplifying weak preexisting magnetic fields, it might be hoped that the character of the magnetic field in accretion disks is independent of the nature of the seed field. However, the divergence-free nature of magnetic fields in highly conducting fluids ensures that their large-scale topology is preserved, no matter how greatly the field intensity is changed. By performing global two-dimensional and three-dimensional general relativistic magnetohydrodynamic disk simulations with several different topologies for the initial magnetic field, we explore the degree to which the character of the flows around black holes depends on the initial topology. We find that while the qualitative properties of the accretion flow are nearly independent of field topology, jet-launching is very sensitive to it: a sense of vertical field consistent for at least an inner disk inflow time is essential to the support of strong jets.
Beckwith Kris
Hawley John F.
Krolik Julian H.
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