4.1 Numerical evolution of equilibrium Rotating Stars in Relativity3.5 Nonaxisymmetric instabilities

4 Rotating Stars in Numerical Relativity

Recently, the dynamical evolution of rapidly rotating stars has become possible in numerical relativity. In the framework of the 3+1 split of the Einstein equations [284], a stationary axisymmetric star can be described by a metric of the standard form

equation1351

where tex2html_wrap_inline4922 is the lapse function, tex2html_wrap_inline4924 is the shift three-vector, and tex2html_wrap_inline4926 is the spatial three-metric, with tex2html_wrap_inline4928 . The spacetime has the following properties:

Crucial ingredients for the successful long-term evolutions of rotating stars in numerical relativity are the conformal ADM schemes for the spacetime evolution (see [234, 277, 32, 4]) and hydrodynamical schemes that have been shown to preserve well the sharp rotational profile at the surface of the star [106Jump To The Next Citation Point In The Article, 294Jump To The Next Citation Point In The Article, 105Jump To The Next Citation Point In The Article].





4.1 Numerical evolution of equilibrium Rotating Stars in Relativity3.5 Nonaxisymmetric instabilities

image Rotating Stars in Relativity
Nikolaos Stergioulas
http://www.livingreviews.org/lrr-2003-3
© Max-Planck-Gesellschaft. ISSN 1433-8351
Problems/Comments to livrev@aei.mpg.de