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arXiv · 0706.0904

Reducing eccentricity in black-hole binary evolutions with initial parameters from post-Newtonian inspiral

Sascha Husa·Mark Hannam·Jose A. Gonzalez·Ulrich Sperhake·Bernd Bruegmann
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Abstract

Standard choices of quasi-circular orbit parameters for black-hole binary evolutions result in eccentric inspiral. We introduce a conceptually simple method, which is to integrate the post-Newtonian equations of motion through hundreds of orbits, and read off the values of the momenta at the separation at which we wish to start a fully general relativistic numerical evolution. For the particular case of non-spinning equal-mass inspiral with an initial coordinate separation of $D = 11M$ we show that this approach reduces the eccentricity by at least a factor of five to $e < 0.002$ as compared to using standard quasi-circular initial parameters.

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Sascha Husa, Mark Hannam, Jose A. Gonzalez, Ulrich Sperhake, Bernd Bruegmann. 2007-06-07. Reducing eccentricity in black-hole binary evolutions with initial parameters from post-Newtonian inspiral. https://doi.org/10.1103/physrevd.77.044037

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