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

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

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

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

Lior Burko, UAH

(work w/ Gaurav Khanna, UMassD)

MWRM-16

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.

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.

elliptical

p=5M e=0.5

parabolic

p=5.828M e=1

Kerr equatorial orbits with a/M=0.5

Waveforms

Upper panel (A): The dominant mode (m=2)

Lower panel (B): The mode m=3

Total energy flux

Dominant mode (m=2)

m=3

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