W-Modes in Rotating Relativistic Stars

Details W-Modes in Rotating Relativistic Stars W-Modes in Rotating Relativistic Stars

Aug 2006

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2006aipc..848..730s&link_type=abstract

RECENT ADVANCES IN ASTRONOMY AND ASTROPHYSICS: 7th International Conference of the Hellenic Astronomical Society. AIP Conferenc

Physics

Stellar Rotation, Wave Generation And Sources, Physics Of Black Holes, Black Holes

Scientific paper

We obtain w-mode frequencies of rapidly rotating, relativistic stars, using a 3D fully nonlinear numerical code. The so-called ``inverse-Cowling approximation'' is used by fixing the evolution of the fluid and allowing only for spacetime dynamics. We demonstrate that in the nonrotating limit the code reproduces known w-mode frequencies obtained through perturbative methods. In the rotating case, we focus on a dynamically unstable model and show that its w-mode frequencies agree well with the gravitational-wave spectrum produced during the initial phase of the dynamical collapse to a Kerr black hole.

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