Abstract
We model the adiabatic inspirai 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 inspirai 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 inspirai wavetrain computed with our QE numerical scheme can be matched to the subsequent plunge and merger waveform calculated with a fully relativistic hydrodynamics code.
Original language | English (US) |
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Article number | 024016 |
Journal | Physical Review D |
Volume | 65 |
Issue number | 2 |
DOIs | |
State | Published - 2002 |
ASJC Scopus subject areas
- Physics and Astronomy (miscellaneous)