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This work introduces a novel formalism to investigate the role of the spin ofastrophysical black holes in determining the behaviour of matter falling ontosuch accretors. Equations describing the general relativistic hydrodynamicaccretion flow in the Kerr metric are formulated, and stationary solutions forsuch flow equations are provided. The accreting matter may becomemulti-transonic, allowing a stationary shock to form for certain initialboundary conditions. Such a shock determines the disc geometry and can drivestrong outflows. The properties of matter extremely close to the event horizonare studied as a function of the Kerr parameter, leading to the possibility ofdetecting a new spectral signature of black hole spin.

Behaviour of relativistic black hole accretion sufficiently close to the horizon