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Accurate time-domain gravitational waveforms for extreme-mass-ratio binaries

Accurate time-domain gravitational waveforms for extreme-mass-ratio binaries. Lior Burko, UAH (work w/ Gaurav Khanna, UMassD). Comparison of GW total energy fluxes. Circular equatorial orbit in Schwarzschild at 18M; Wave extraction done at 500M.

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Accurate time-domain gravitational waveforms for extreme-mass-ratio binaries

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  1. Accurate time-domain gravitational waveforms for extreme-mass-ratio binaries Lior Burko, UAH (work w/ Gaurav Khanna, UMassD) MWRM-16

  2. Comparison of GW total energy fluxes Circular equatorial orbit in Schwarzschild at 18M; Wave extraction done at 500M. Circular equatorial orbit in Kerr (a/M=0.9) at ; Wave extraction at 500M.

  3. The relative error in the energy flux in gravitational waves • Particle in circular and equatorial orbit in Kerr (a/m=0.5) • Grid density is 0.025M (radial) x 0.05 (angular) • Particle is modeled with a gaussian Upper panel (A): As a function of the distance at which wave extraction is done. The errors are calculated with a value corresponding to wave extraction at infinity, that we obtain using Richardson's extrapolations. Here, N=5. Lower panel (B): As a function of the number of points used to sample the Gaussian N. The errors are calculated with the FD value. Wave extraction is done at 500M.

  4. Zoom - Whirl orbits elliptical p=5M e=0.5 parabolic p=5.828M e=1 Kerr equatorial orbits with a/M=0.5

  5. Elliptical orbit Waveforms Upper panel (A): The dominant mode (m=2) Lower panel (B): The mode m=3 Total energy flux

  6. Parabolic orbit Dominant mode (m=2) m=3

  7. Parabolic orbit Characteristic strain in GW 1 - 10^6 solar masses BHs Central BH has a/M=0.5 Distance 1 Gpc Standard LISA noise curve with SNR=1 Total energy flux

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