Figure 14: Relativistic wind accretion onto a rapidly-rotating Kerr black hole ( ,
the black-hole spin is counterclockwise) in Kerr–Schild coordinates (left panel). Isocontours of the
logarithm of the density are plotted at the final stationary time . Brighter colors
(yellow-white) indicate high density regions, while darker colors (blue) correspond to low density
zones. The right panel shows how the flow solution looks when transformed to Boyer–Lindquist
coordinates. The shock appears here totally wrapped around the horizon of the black hole. The box
is units long. The simulation employed a -grid of zones. Further details
are given in [135].
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