Astronomy and Astrophysics – Astronomy
Scientific paper
May 1995
adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1995aas...186.4812h&link_type=abstract
American Astronomical Society, 186th AAS Meeting, #48.12; Bulletin of the American Astronomical Society, Vol. 27, p.880
Astronomy and Astrophysics
Astronomy
Scientific paper
We present 3D numerical simulations of the non-axisymmetric dynamical bar mode instability in a rotating star, as well as the resulting gravitational radiation waveforms. This instability may operate during the collapse of rapidly rotating stellar cores or in white dwarfs spun up by accretion. Using a smoothed particle hydrodynamics (SPH) code, we created 7 models, varying the number of particles used to represent the fluid, the artificial viscosity, and the type of initial model distribution. We here compare the resulting growth rates, bar rotation speeds, mass and angular momentum distributions, and gravitational radiation quantities. The star was modeled as a polytrope with index n = 3/2, and starts out with T_rot/|W| ~ 0.30, where T_rot is the rotational kinetic energy and |W| is the gravitational potential energy. The code assumes a Newtonian gravitational field, and the gravitational radiation is calculated in the quadrupole approximation. The conclusion of this analysis shows that all models deform into a bar shape and shed mass in the form of a two-armed spiral pattern. Typically, ~ 10% of the original mass and ~ 30% of the original angular momentum are transferred to the arms, which eventually spread into a uniform quasi-Keplerian disk. The resulting central core rotates with T_rot/|W| ~ 0.25, just below the dynamical instability point. Finally, the amplitudes of the gravitational wave quantities increase as the number of particles increases. Higher resolution runs, or models with non-equal-mass particles are needed to achieve convergence in these quantities.
Centrella Joan M.
Houser Janet L.
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