In a magnetized viscous accretion disk model, adding saturated thermal conduction and thermal-driven winds moves the standing shock outward from the black hole and shrinks the parameter space for shock solutions, offering a qualitative explanation for the declining QPO frequencies in black hole…
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A generic iterative shooting algorithm locates all classes of global transonic accretion and wind solutions, including shocked solutions, around compact objects.
Viscous transonic accretion flow simulations around spinning black holes show that QPO frequency ranges and power-law photon indices correlate with black hole spin.
Winds in shocked magnetized viscous accretion flows around rotating black holes reduce luminosity, modify shock radius, compression, and strength, and impose a critical wind parameter p^crit above which steady shocks cease to exist.
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QPOs from the Viscous Transonic Accretion Flow Around a Spinning Black Hole
Viscous transonic accretion flow simulations around spinning black holes show that QPO frequency ranges and power-law photon indices correlate with black hole spin.
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Influence of winds on shocked magnetized viscous accretion flows around rotating black holes
Winds in shocked magnetized viscous accretion flows around rotating black holes reduce luminosity, modify shock radius, compression, and strength, and impose a critical wind parameter p^crit above which steady shocks cease to exist.