Accurate time-domain gravitational
waveforms for extreme-mass-ratio
Lior Burko, UAH
(work w/ Gaurav Khanna, UMassD)
November 17, 2006 MWRM-16
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.
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
•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.
Zoom - Whirl orbits
p=5M e=0.5 p=5.828M e=1
Kerr equatorial orbits with a/M=0.5
Waveforms Total energy flux
Upper panel (A): The dominant
Lower panel (B): The mode m=3
Dominant mode (m=2) m=3
Characteristic strain in GW
Total energy flux
1 - 10^6 solar masses BHs
Central BH has a/M=0.5
Distance 1 Gpc
Standard LISA noise curve with SNR=1