Fundamental physics with LISA

Schutz, B. F.

doi:10.1088/0264-9381/26/9/094020

Cited by 22 publications

(33 citation statements)

References 28 publications

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“…Because at large radii F 2 (r) ≈ −F 1 (r) ≈ (M/r) 3 , we see that the deformation h µν , when inserted in the Hamiltonian (5.43), gives the correct leading-order (2PN) coupling of the particle's spin with itself. Keeping only the leading-order term created by h µν , the effective EOB Hamiltonian therefore becomes…”

Section: Discussionmentioning

confidence: 83%

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Improved effective-one-body Hamiltonian for spinning black-hole binaries

2010

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Building on a recent paper in which we computed the canonical Hamiltonian of a spinning test particle in curved spacetime, at linear order in the particle's spin, we work out an improved effectiveone-body (EOB) Hamiltonian for spinning black-hole binaries. As in previous descriptions, we endow the effective particle not only with a mass µ, but also with a spin S * . Thus, the effective particle interacts with the effective Kerr background (having spin SKerr) through a geodesic-type interaction and an additional spin-dependent interaction proportional to S * . When expanded in post-Newtonian (PN) orders, the EOB Hamiltonian reproduces the leading order spin-spin coupling and the spin-orbit coupling through 2.5PN order, for any mass-ratio. Also, it reproduces all spinorbit couplings in the test-particle limit. Similarly to the test-particle limit case, when we restrict the EOB dynamics to spins aligned or antialigned with the orbital angular momentum, for which circular orbits exist, the EOB dynamics has several interesting features, such as the existence of an innermost stable circular orbit, a photon circular orbit, and a maximum in the orbital frequency during the plunge subsequent to the inspiral. These properties are crucial for reproducing the dynamics and gravitational-wave emission of spinning black-hole binaries, as calculated in numerical relativity simulations.

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Section: Discussionmentioning

confidence: 83%

“…Coalescing black-hole binaries are among the most promising sources for the current and future laserinterferometer gravitational-wave detectors, such as the ground-based detectors LIGO and Virgo [1,2] and the space-based detector LISA [3].…”

Section: Introductionmentioning

confidence: 99%

Improved effective-one-body Hamiltonian for spinning black-hole binaries

2010

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“…Using this alignment procedure, we estimate the errors on the numerical É 22 4 . Figures 1 and 2 summarize the phase errors for numerical É 22 4 . The numerical waveform labeled ''(N6,…”

Section: A Uncertainties In Numerical Waveformsmentioning

confidence: 99%

“…We expect that in the future, the peak amplitude of the numerical h 22 will be predicted by numerical relativity with high accuracy as an interpolation function on the physical parameters. Therefore, a 4 , are calibrated to the numerical waveform to further reduce the disagreement in amplitude. The NQC parameters will enter the flux through the NQC waveform NQC h 22 in the next iteration.…”

Section: B Calibrating the Eob-adjustable Parametersmentioning

confidence: 99%

Effective-one-body waveforms calibrated to numerical relativity simulations: Coalescence of nonprecessing, spinning, equal-mass black holes

et al. 2010

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We present the first attempt at calibrating the effective-one-body (EOB) model to accurate numerical relativity simulations of spinning, nonprecessing black-hole binaries. Aligning the EOB and numerical waveforms at low frequency over a time interval of 1000M, we first estimate the phase and amplitude errors in the numerical waveforms and then minimize the difference between numerical and EOB waveforms by calibrating a handful of EOB-adjustable parameters. In the equal-mass, spin aligned case, we find that phase and fractional amplitude differences between the numerical and EOB ð2; 2Þ mode can be reduced to 0.01 radian and 1%, respectively, over the entire inspiral waveforms. In the equal-mass, spin antialigned case, these differences can be reduced to 0.13 radian and 1% during inspiral and plunge, and to 0.4 radian and 10% during merger and ringdown. The waveform agreement is within numerical errors in the spin aligned case while slightly over numerical errors in the spin antialigned case. Using Enhanced LIGO and Advanced LIGO noise curves, we find that the overlap between the EOB and the numerical ð2; 2Þ mode, maximized over the initial phase and time of arrival, is larger than 0.999 for binaries with total mass 30M -200M . In addition to the leading ð2; 2Þ mode, we compare four subleading modes. We find good amplitude and frequency agreements between the EOB and numerical modes for both spin configurations considered, except for the ð3; 2Þ mode in the spin antialigned case. We believe that the larger difference in the ð3; 2Þ mode is due to the lack of knowledge of post-Newtonian spin effects in the higher modes.

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“…It is to carry out detailed studies of whether the observed merger signals are in complete agreement with the predictions of general relativity (see e.g., [Schutz (2009a)]). For MBH binary mergers with comparable masses, advances in numerical relativity in the last few years indicate that accurate general relativistic templates for the signals will be available by the time they are needed, even for the merger and ringdown phases of the process.…”

Section: Primary Scientific Objectives Of Lisamentioning

confidence: 99%

Gravitational wave astronomy, relativity tests, and massive black holes

Bender

2009

Proc. IAU

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Abstract. The gravitational wave detectors that are operating now are looking for several kinds of gravitational wave signals at frequencies of tens of Hertz to kilohertz. One of these is mergers of roughly 10 M BH binaries. Sometime between now and about 8 years from now, it is likely that signals of this kind will be observed. The result will be strong tests of the dynamical predictions of general relativity in the high field regime. However, observations at frequencies below 1 Hz will have to wait until the launch of the Laser Interferometer Space Antenna (LISA), hopefully only a few years later. LISA will have 3 main objectives, all involving massive BHs. The first is observations of mergers of pairs of intermediate mass (100 to 10 5 M ) and higher mass BHs at redshifts out to roughly z=10. This will provide new information on the initial formation and growth of BHs such as those found in most galaxies, and the relation between BH growth and the evolution of galactic structure. The second objective is observations of roughly 10 M BHs, neutron stars, and white dwarfs spiraling into much more massive BHs in galactic nuclei. Such events will provide detailed information on the populations of such compact objects in the regions around galactic centers. And the third objective is the use of the first two types of observations for testing general relativity even more strongly than ground based detectors will. As an example, an extreme mass ratio event such as a 10 M BH spiraling into a galactic center BH can give roughly 10 5 observable cycles during about the last year before merger, with a mean relative velocity of 1/3 to 1/2 the speed of light, and the frequencies of periapsis precession and Lense-Thirring precession will be high. The LISA Pathfinder mission to prepare for LISA is scheduled for launch in 2011.

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Fundamental physics with LISA

Cited by 22 publications

References 28 publications

Improved effective-one-body Hamiltonian for spinning black-hole binaries

Improved effective-one-body Hamiltonian for spinning black-hole binaries

Effective-one-body waveforms calibrated to numerical relativity simulations: Coalescence of nonprecessing, spinning, equal-mass black holes

Gravitational wave astronomy, relativity tests, and massive black holes

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