Gravitational radiation from the bar mode instability in differentially rotating polytropes

Details Gravitational radiation from the bar mode instability in differentially rotating polytropes Gravitational radiation from the bar mode instability in differentially rotating polytropes

Jan 1993

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1993phdt........63s&link_type=abstract

PhD Dissertation, Drexel Univ. Philadelphia, PA United States

Physics

3

Gravitational Waves, Polytropic Processes, Neutron Stars, Hydrodynamics, Stellar Models, Self Consistent Fields, Finite Difference Theory, Angular Momentum, Stellar Mass, Quadrupoles

Scientific paper

We describe the development and use of a 3-D explicit finite difference hydrodynamics code for the study of gravitational radiation emission by the dynamical bar mode instability in a n = 3/2 polytrope with T/(absolute value of W) = 0.3. Newtonian gravity is used, with gravitational radiation calculated in the quadrupole approximation. The differentially rotating initial model is generated using a self consistent field method. The growth rate and eigenfrequency of the bar mode match the predictions of tensor virial equation analysis. The model ejects approximately 4% of its mass and approximately 13% of its angular momentum in the form of spiral arms, which ultimately merge to form a tenuous envelope surrounding a dense core and extending to a radius approximately 2.2 times the initial radius. We find that a typical neutron star will radiate approximately 0.36% of its mass and approximately 4.5% of its angular momentum in the form of gravitational radiation. The characteristic frequency of these waves will be approximately 4 kHz, and the dimensionless amplitude will be h is approximately 4.6 x 10-22 at the distance of the Virgo Cluster.

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