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Area of Science:

  • Astrophysics
  • General Relativity
  • Gravitational Waves

Background:

  • General relativity predicts gravitational wave (GW) signatures from coalescing binary black holes.
  • Post-Newtonian (PN) approximations are the primary method for generating waveform predictions for GW data analysis.
  • The accuracy of PN approximations during the late-inspiral phase remains uncertain.

Purpose of the Study:

  • To derive late-inspiral gravitational waveforms using direct numerical simulations of Einstein's equations.
  • To compare the phasing of waveforms from numerical simulations with PN approximations.
  • To assess the effectiveness of PN approximations in the crucial late-inspiral phase.

Main Methods:

  • Direct numerical simulation of Einstein's field equations for binary black hole mergers.
  • Comparison of waveform phasing between numerical relativity simulations and post-Newtonian (PN) approximations (2.5PN, 3PN, 3.5PN).
  • Focus on the last approximately 14 cycles of gravitational radiation from equal-mass, nonspinning black holes.

Main Results:

  • Waveform phasing from numerical simulations shows agreement with 2.5PN, 3PN, and 3.5PN approximations.
  • The agreement is consistent with the internal error estimates of both simulation methods.
  • Post-Newtonian approximations remain effective until the final orbit before merger.

Conclusions:

  • Numerical relativity simulations provide a complementary approach to PN approximations for binary black hole mergers.
  • Post-Newtonian approximations are reliable for analyzing gravitational wave data until the very end of the inspiral phase.
  • This study validates the use of PN waveforms for a significant portion of the late-inspiral signal.