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Accurate time-domain gravitational waveforms for extreme-mass

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Accurate time-domain gravitational waveforms for extreme-mass Powered By Docstoc
					      Accurate time-domain gravitational
      waveforms for extreme-mass-ratio
                      binaries


                    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.



                                                                                        2
                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.
                                                                                                      3
             Zoom - Whirl orbits




elliptical                     parabolic
p=5M         e=0.5             p=5.828M e=1

Kerr equatorial orbits with a/M=0.5
                                              4
                          Elliptical orbit




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




Dominant mode (m=2)                     m=3




                                              6
                    Parabolic orbit




                            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
                                                            7

				
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posted:4/12/2013
language:English
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