Other
Scientific paper
May 2004
adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2004aps..apr.l3004d&link_type=abstract
American Physical Society, April Meeting, 2004, May 1-4, 2004, Denver, Colorado April 2004, MEETING ID: APR04, abstract #L3.004
Other
Scientific paper
Accretion onto black holes is thought to produce astrophysically important effects in two broad classes of systems: X-ray binaries, where one companion is a black hole in the stellar mass range, and in active galaxies, where million- to billion-solar mass black holes at their center are thought to drive the wide range of phenomena, notably highly collimated jets, associated with Active Galactic Nuclei (AGNs). Numerical methods hold the key to deepening our theoretical understanding of such systems, but many challenges present themselves since numerical studies require large-scale simulations of magnetized fluids in the curved spacetime of a rotating black hole. Recently, a fully relativistic 3D MHD code has been applied to this problem. In the simulations discussed here, a unified picture is beginning to emerge wherein accretion from a magnetized gas torus leads to the self-consistent launching of jets in the vicinity of the black hole. Accretion is driven by the Balbus-Hawley instability, which generates the turbulent motions responsible for outward transport of angular momentum by amplifying a seed magnetic field through orbital shear. Close to the black hole's marginally stable orbit, steep pressure gradients and the Lorentz force act on matter piling up near the accretion throat to launch jets along the funnel wall. The intensity of the jets, and other observable effects, can be enhanced by energy extraction processes if the black hole is spinning.
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