Physics
Scientific paper
May 1996
adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1996aps..may.j1503h&link_type=abstract
American Physical Society, APS/AAPT Joint Meeting, May 2-5, 1996, abstract #J15.03
Physics
Scientific paper
We present 3D numerical simulations of the nonaxisymmetric dynamical bar mode instability in rotating stars, as well as the resulting gravitational waveforms. This instability may operate during the collapse of rapidly rotating stellar cores or in compact objects spun up by accretion. Using a smoothed particle hydrodynamics (SPH) code, we have investigated the effects of the ``stiffness'' of the polytropic equation of state on the gravitational wave quantities and the bar growth rate and pattern speed. The star initially has T_rot/|W| ≈ 0.30, where T_rot is the rotational kinetic energy and W is the gravitational potential energy. The rotation law imposed is that for uniformly rotating, constant density Maclaurin spheroids; when applied to polytropes this produces differential rotation. The code uses a Newtonian gravitational field, and the gravitational radiation is calculated in the quadrupole approximation. This research is supported by NSF grant PHY--9208914, and the simulations were carried out at the Pittsburgh Supercomputing Center.
Centrella Joan M.
Houser Janet L.
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