Effective-one-body waveforms from dynamical captures in black hole binaries

  title={Effective-one-body waveforms from dynamical captures in black hole binaries},
  author={A. Nagar and Piero Rettegno and Rossella Gamba and Sebastiano Bernuzzi},
  journal={arXiv: General Relativity and Quantum Cosmology},
Dynamical capture is a possible formation channel for BBH mergers leading to highly eccentric merger dynamics and to gravitational wave (GW) signals that are morphologically different from those of quasi-circular mergers. The future detection of these mergers by ground-based or space-based GW interferometers can provide invaluable insights on astrophysical black holes, but it requires precise predictions and dedicated waveform models for the analysis. We present a state-of-the-art effective-one… 

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and F

  • Messina,
  • 2020


  • Rev. D87, 043004
  • 2013


  • Rev. D 101, 101501
  • 2020

and R

  • Gamba,
  • 2019

and a at

The xishacorene natural products are structurally unique apolar diterpenoids that feature a bicyclo[3.3.1] framework. These secondary metabolites likely arise from the well-studied, structurally

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