Gravitational wave snapshots of generic extreme mass ratio inspirals

Drasco, Steve; Hughes, Scott A.

doi:10.1103/physrevd.73.024027

Cited by 208 publications

(201 citation statements)

References 69 publications

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“…These computations have recently been extended to fully generic orbits [37,38,39]. However first order perturbation theory is limited to producing "snapshot" waveforms that neglect radiation reaction.…”

Section: B Methods Of Computing Orbital Motion and Waveformsmentioning

confidence: 99%

Two-timescale analysis of extreme mass ratio inspirals in Kerr spacetime: Orbital motion

2008

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Inspirals of stellar mass compact objects into massive black holes are an important source for future gravitational wave detectors such as Advanced LIGO and LISA. Detection of these sources and extracting information from the signal relies on accurate theoretical models of the binary dynamics. We cast the equations describing binary inspiral in the extreme mass ratio limit in terms of action angle variables, and derive properties of general solutions using a two-timescale expansion. This provides a rigorous derivation of the prescription for computing the leading order orbital motion. As shown by Mino, this leading order or adiabatic motion requires only knowledge of the orbit-averaged, dissipative piece of the self force. The two timescale method also gives a framework for calculating the post-adiabatic corrections. For circular and for equatorial orbits, the leading order corrections are suppressed by one power of the mass ratio, and give rise to phase errors of order unity over a complete inspiral through the relativistic regime. These post-1-adiabatic corrections are generated by the fluctuating, dissipative piece of the first order self force, by the conservative piece of the first order self force, and by the orbit-averaged, dissipative piece of the second order self force. We also sketch a two-timescale expansion of the Einstein equation, and deduce an analytic formula for the leading order, adiabatic gravitational waveforms generated by an inspiral.

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Section: B Methods Of Computing Orbital Motion and Waveformsmentioning

confidence: 99%

Two-timescale analysis of extreme mass ratio inspirals in Kerr spacetime: Orbital motion

2008

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“…Ones can also solve it through some analytical method [40] or post-Newtonian approximation [41]. In [42], the authors used geodesic equation to treat the eccentric orbit of a large mass ratio binary and used the Teukolsky equation to treat the waveform problem. Interestingly, people have used the method of geodesic equation and Teukolsky equation to find that the eccentricity may increase [43,44] instead of always decay found through post-Newtonian approximation [19].…”

Section: Introductionmentioning

confidence: 99%

Waveform model for an eccentric binary black hole based on the effective-one-body-numerical-relativity formalism

Cao¹,

Han²

2017

Phys. Rev. D

150

134

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Binary black hole systems are among the most important sources for gravitational wave detection. And also they are good objects for theoretical research for general relativity. Gravitational waveform template is important to data analysis. Effective-one-body-numerical-relativity (EOBNR) model has played an essential role in the LIGO data analysis. For future space-based gravitational wave detection, many binary systems will admit somewhat orbit eccentricity. At the same time the eccentric binary is also an interesting topic for theoretical study in general relativity. In this paper we construct the first eccentric binary waveform model based on effective-one-body-numerical-relativity framework. Our basic assumption in the model construction is that the involved eccentricity is small. We have compared our eccentric EOBNR model to the circular one used in LIGO data analysis. We have also tested our eccentric EOBNR model against to another recently proposed eccentric binary waveform model; against to numerical relativity simulation results; and against to perturbation approximation results for extreme mass ratio binary systems. Compared to numerical relativity simulations with eccentricity as large as about 0.2, the overlap factor for our eccentric EOBNR model is better than 0.98 for all tested cases including spinless binary and spinning binary; equal mass binary and unequal mass binary. Hopefully our eccentric model can be the start point to develop a faithful template for future space-based gravitational wave detectors.

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“…In this section we review the derivation of the harmonic decomposition (8.8) given by Drasco and Hughes [42,51], adapted to the scalar case, and generalized from fiducial geodesics to arbitrary bound geodesics. We consider only the "out" amplitude Z out ωlm ; the "down" case is exactly analogous.…”

Section: Harmonic Decomposition Of Amplitudesmentioning

confidence: 99%

“…For the case considered here where the source T (x) is a point particle on a bound geodesic orbit, the amplitudes Z out ωlm and Z down ωlm can be expressed as discrete sums over delta functions [42,51]:…”

Section: Harmonic Decomposition Of Amplitudesmentioning

confidence: 99%

Computing inspirals in Kerr in the adiabatic regime: I. The scalar case

Drasco

Flanagan

Hughes

2005

Class. Quantum Grav.

Self Cite

185

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Abstract.A key source for LISA will be the inspiral of compact objects into massive black holes. Recently Mino has shown that in the adiabatic limit, gravitational waveforms for these sources can be computed by using for the radiation reaction force the gradient of one half the difference between the retarded and advanced metric perturbations. Using post-Newtonian expansions, we argue that the resulting waveforms should be sufficiently accurate for signal detection with LISA. Data-analysis templates will require higher accuracy, going beyond adiabaticity; this remains a significant challenge.We describe an explicit computational procedure for obtaining waveforms based on Mino's result, for the case of a point particle coupled to a scalar field. We derive an explicit expression for the time-averaged time derivative of the Carter constant, and verify that the expression correctly predicts that circular orbits remain circular while evolving under the influence of radiation reaction. The derivation uses detailed properties of mode expansions, Green's functions and bound geodesic orbits in the Kerr spacetime, which we review in detail. This paper is about three quarters review and one quarter new material. The intent is to give a complete and self-contained treatment of scalar radiation reaction in the Kerr spacetime, in a single unified notation, starting with the Kerr metric, and ending with formulae for the time evolution of all three constants of the motion that are sufficiently explicit to be used immediately in a numerical code.

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Gravitational wave snapshots of generic extreme mass ratio inspirals

Cited by 208 publications

References 69 publications

Two-timescale analysis of extreme mass ratio inspirals in Kerr spacetime: Orbital motion

Two-timescale analysis of extreme mass ratio inspirals in Kerr spacetime: Orbital motion

Waveform model for an eccentric binary black hole based on the effective-one-body-numerical-relativity formalism

Computing inspirals in Kerr in the adiabatic regime: I. The scalar case

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