
Abstract 
1 
Introduction 

1.1 
Overview of BHNS binaries 

1.2 
Tidal problem around
a BH: Effects of BH spin and the NS EOS 

1.3 
Why is the merger of
BHNS binaries important? 

1.4 
General relativistic study of BHNS
binaries in quasiequilibrium states 

1.5 
Nonrelativistic simulation for the
merger 

1.6 
Stable mass transfer occurs or not 

1.7 
General relativistic study
of late inspiral and merger 

1.8 
Outline and notation 
2 
QuasiEquilibrium
States 

2.1 
Formulation 

2.2 
Current parameter space surveyed 

2.3 
Numerical
results 

2.4 
Endpoint of sequences 

2.5 
Summary: quasiequilibrium
states 
3 
Numerical Simulations 

3.1 
Numerical method 

3.2 
Current parameter
space surveyed 

3.3 
Merger process 

3.4 
Properties of the remnant black hole
and disk 

3.5 
Criteria for tidal disruption 

3.6 
Gravitational waveforms 

3.7 
The
Fourier spectrum of gravitational waves 

3.8 
Summary and issues for
the near future 
4 
Acknowledgements 
A 
Basic Field Equations 

References 

Footnotes 

Figures 

Tables 