
Abstract 
1 
Introduction 
2 
Three Destinations in Kerr’s Strong Gravity 

2.1 
The
event horizon 

2.2 
The ergosphere 

2.3 
ISCO: the orbit of marginal
stability 

2.4 
The Paczyński–Wiita potential 

2.5 
Summary: characteristic
radii and frequencies 
3 
Matter Description: General Principles 

3.1 
The
fluid part 

3.2 
The stress part 

3.3 
The Maxwell part 

3.4 
The radiation
part 
4 
Thick Disks, Polish Doughnuts, & Magnetized Tori 

4.1 
Polish
doughnuts 

4.2 
Magnetized Tori 
5 
Thin Disks 

5.1 
Equations in the Kerr
geometry 

5.2 
The eigenvalue problem 

5.3 
Solutions: Shakura–Sunyaev &
Novikov–Thorne 
6 
Slim Disks 
7 
AdvectionDominated Accretion Flows
(ADAFs) 
8 
Stability 

8.1 
Hydrodynamic stability 

8.2 
Magnetorotational
instability (MRI) 

8.3 
Thermal and viscous instability 
9 
Oscillations 

9.1 
Dynamical
oscillations of thick disks 

9.2 
Diskoseismology: oscillations of thin
disks 
10 
Relativistic Jets 
11 
Numerical Simulations 

11.1 
Numerical
techniques 

11.2 
Matter description in simulations 

11.3 
Polish doughnuts
(thick) disks in simulations 

11.4 
Novikov–Thorne (thin) disks in
simulations 

11.5 
ADAFs in simulations 

11.6 
Oscillations in simulations 

11.7 
Jets
in simulations 

11.8 
Highly magnetized accretion in simulations 
12 
Selected
Astrophysical Applications 

12.1 
Measurements of blackhole mass and
spin 

12.2 
Black hole vs. neutron star accretion disks 

12.3 
Blackhole accretion
disk spectral states 

12.4 
QuasiPeriodic Oscillations (QPOs) 

12.5 
The
case of Sgr A* 
13 
Concluding Remarks 
14 
Acknowledgements 

References 

Footnotes 

Figures 

Tables 