1 Introduction

Rotating Stars in Relativity

Update available: http://www.livingreviews.org/lrr-2003-3

Nikolaos Stergioulas

Department of Physics, University of Wisconsin-Milwaukee
PO Box 413, Milwaukee, WI 53201, USA
Max Planck Institute for Gravitational Physics
D-14473 Potsdam, Germany
email: niksterg@aei-potsdam.mpg.de

(Accepted 28 May 1998)
(Last Amended 31 August 2001 Jump To The First Amendment In The Article)


Because of the information they can yield about the equation of state of matter at extremely high densities and because they are one of the more possible sources of detectable gravitational waves, rotating relativistic stars have been receiving significant attention in recent years. We review the latest theoretical and numerical methods for modeling rotating relativistic stars, including stars with a strong magnetic field and hot proto-neutron stars. We also review nonaxisymmetric oscillations and instabilities in rotating stars and summarize the latest developments regarding the gravitational wave-driven (CFS) instability in both polar and axial quasi-normal modes.

1 Introduction

image Rotating Stars in Relativity
Nikolaos Stergioulas
© Max-Planck-Gesellschaft. ISSN 1433-8351
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