Instability of Rapidly Rotating Compact Stellar Cores

Details Instability of Rapidly Rotating Compact Stellar Cores Instability of Rapidly Rotating Compact Stellar Cores

Apr 2000

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2000aps..aprq20008c&link_type=abstract

American Physical Society, April Meeting, April 29-May 2, 2000 Long Beach, CA, abstract #Q20.008

Physics

Scientific paper

One interesting class of gravitational wave sources encompasses rapidly rotating stellar cores that have expended their nuclear fuel and are prevented from undergoing further collapse by centrifugal forces. The development of global rotational instabilities in such a ``centrifugally-hung'' object can produce gravitational radiation and may shed enough angular momentum to allow full collapse to a supernova. We are using 3-D numerical simulations to investigate the stability of rotating stellar cores modeled as polytropes with N > 3 for various rotation laws. The hydrocode calculates the gravitational field in the Newtonian limit, and the resulting gravitational radiation is computed in the quadrupole approximation. In certain cases we find that such cores can be unstable at values of β = T/|W| considerably lower than the Maclaurin limit βd ≈ 0.27 for the dynamical bar instability.

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