1 / 7

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.

awena
Télécharger la présentation

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

An Image/Link below is provided (as is) to download presentation Download Policy: Content on the Website is provided to you AS IS for your information and personal use and may not be sold / licensed / shared on other websites without getting consent from its author. Content is provided to you AS IS for your information and personal use only. Download presentation by click this link. While downloading, if for some reason you are not able to download a presentation, the publisher may have deleted the file from their server. During download, if you can't get a presentation, the file might be deleted by the publisher.

E N D

Presentation Transcript

  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

More Related