Isothermal Shock Formation in Non-Equatorial Accretion Flows around Kerr Black Holes

Details Isothermal Shock Formation in Non-Equatorial Accretion Flows around Kerr Black Holes Isothermal Shock Formation in Non-Equatorial Accretion Flows around Kerr Black Holes

2004-05-13

arxiv.org/abs/astro-ph/0405269v1

Astrophys.J. 611 (2004) 964-976

Astronomy and Astrophysics

Astrophysics

22 pages with 11 figures, presented at 5th international conference on high energy density laboratory astrophysics in Tucson,

Scientific paper

10.1086/422243

We explore isothermal shock formation in non-equatorial, adiabatic accretion flows onto a rotating black hole, with possible application to some active galactic nuclei (AGNs). The isothermal shock jump conditions as well as the regularity condition, previously developed for one-dimensional (1D) flows in the equatorial plane, are extended to two-dimensional (2D), non-equatorial flows, to explore possible geometrical effects. The basic hydrodynamic equations with these conditions are self-consistently solved in the context of general relativity to explore the formation of stable isothermal shocks. We find that strong shocks are formed in various locations above the equatorial plane, especially around a rapidly-rotating black hole with the prograde flows (rather than a Schwarzschild black hole). The retrograde flows are generally found to develop weaker shocks. The energy dissipation across the shock in the hot non-equatorial flows above the cooler accretion disk may offer an attractive illuminating source for the reprocessed features, such as the iron fluorescence lines, which are often observed in some AGNs.

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