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Comparing the inspiral of irrotational and corotational binary neutron stars

Matthew D. Duez·Thomas W. Baumgarte·Stuart L. Shapiro·Masaru Shibata·Koji Uryu
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Abstract

We model the adiabatic inspiral of relativistic binary neutron stars in a quasi-equilibrium (QE) approximation, and compute the gravitational wavetrain from the late phase of the inspiral. We compare corotational and irrotational sequences and find a significant difference in the inspiral rate, which is almost entirely caused by differences in the binding energy. We also compare our results with those of a point-mass post-Newtonian calculation. We illustrate how the late inspiral wavetrain computed with our QE numerical scheme can be matched to the subsequent plunge and merger waveform calculated with a fully relativistic hydrodynamics code.

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Matthew D. Duez, Thomas W. Baumgarte, Stuart L. Shapiro, Masaru Shibata, Koji Uryu. 2001-09-30. Comparing the inspiral of irrotational and corotational binary neutron stars. https://doi.org/10.1103/physrevd.65.024016

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