Accurate evolutions of orbiting black-hole binaries without excision.

By M. Campanelli, C. Lousto, P. Marronetti, Yosef Zlochower. Physical Review Letters, 2005

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We present a new algorithm for evolving orbiting black-hole binaries that does not require excision or a corotating shift. Our algorithm is based on a novel technique to handle the singular puncture conformal factor. This system, based on the Baumgarte-Shapiro-Shibata-Nakamura formulation of Einstein's equations, when used with a "precollapsed" initial lapse, is nonsingular at the start of the evolution and remains nonsingular and stable provided that a good choice is made for the gauge. As a test case, we use this technique to fully evolve orbiting black-hole binaries from near the innermost stable circular orbit regime. We show fourth-order convergence of waveforms and compute the radiated gravitational energy and angular momentum from the plunge. These results are in good agreement with those predicted by the Lazarus approach.

Subfields: Astronomy and Astrophysics, Nuclear and High Energy Physics

View Paper: https://www.semanticscholar.org/paper/c9d838a9b576ef12d44406754dee368983a78129

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Citations in the corpus

Physics, Astrophysics and Cosmology with Gravitational Waves (2009, background): “A breakthrough came in early 2005 with Pretorius [298] announcing the results from the first stable simulation ever, followed by further breakthroughs by two other groups [104, 61] with successful simulations.”
Doing Science with eLISA: Astrophysics and Cosmology in the Millihertz Regime (2012, background): “umerical relativity, it became possible to accurately determine the evolution of the initial spins of the black holes to the ﬁnal spin of the remnant black hole in a merger event (Baker et al., 2006, Campanelli et al., 2006, Centrella et al., 2010, Pretorius, 2005, Rezzolla et al., 2008a). Numerical”
Black-hole binaries, gravitational waves, and numerical relativity (2010, methodology): “The nonspinning case is again between these two cases, with Erad ∼ 0.04M and (a/M)f ∼ 0.69 (Campanelli et al., 2006d).”
Black hole formation from axion stars (2016, methodology): “These parameters are specified on the initial hypersurface and then allowed to evolve using gauge-driver equations, in accordance with the puncture gauge [44, 45], for which the evolution equations are”
Gravitational Recoil from Spinning Binary Black Hole Mergers (2007, background): “The minimal resolution found to be adequate for spinning cases according to Campanelli et al. (2006b) is h < M/30.”
Unequal mass binary black hole plunges and gravitational recoil (2006, methodology): “The conformal factor φ is used to set the initial lapse as α = φ−2 [13, 21], while the initial shift is β = 0.”