Gravitational Radiation from Rotational Instabilities

Details Gravitational Radiation from Rotational Instabilities Gravitational Radiation from Rotational Instabilities

Dec 1992

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1992aas...181.2907s&link_type=abstract

American Astronomical Society, 181st AAS Meeting, #29.07D; Bulletin of the American Astronomical Society, Vol. 24, p.1166

Astronomy and Astrophysics

Astrophysics

Scientific paper

A 3-D explicit finite difference Eulerian hydrodynamics code has been developed for the study of astrophysical problems. The code implements Newtonian gravity and hydrodynamics on a non-uniform moving cylindrical grid, and is capable of extracting gravitational radiation waveforms using the standard quadrupole formulation. The code has been extensively tested on a variety of 1-, 2-, and 3-D problems including shock and collapse problems. We have applied the program to the study of the growth of the non-axisymmetric dynamical bar mode instability for a differentially rotating polytrope, and have extracted gravitational radiation waveforms. This instability may operate during the collapse of rapidly rotating stellar cores or in white dwarfs that have been spun up by accretion.

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