Census of transient orbital resonances encountered during binary inspiral

Ruangsri, Uchupol; Hughes, Scott A.

doi:10.1103/physrevd.89.084036

Cited by 48 publications

(60 citation statements)

References 30 publications

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“…Transient resonances in EMRIs are an important consideration in waveform modelling due to the high proportion of expected systems encountering a low-order resonance in the later stages of inspiral [86]. Passing through resonance can lead to an enhancement or decrement in the radiated fluxes associated with orbital evolution, which in turn leads to a jump in the orbital parameters across the resonance.…”

Section: Discussionmentioning

confidence: 99%

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Importance of transient resonances in extreme-mass-ratio inspirals

et al. 2016

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The inspiral of stellar-mass compact objects, like neutron stars or stellar-mass black holes, into supermassive black holes provides a wealth of information about the strong gravitational-field regime via the emission of gravitational waves. In order to detect and analyse these signals, accurate waveform templates which include the effects of the compact object's gravitational self-force are required. For computational efficiency, adiabatic templates are often used. These accurately reproduce orbit-averaged trajectories arising from the first-order self-force, but neglect other effects, such as transient resonances, where the radial and poloidal fundamental frequencies become commensurate. During such resonances the flux of gravitational waves can be diminished or enhanced, leading to a shift in the compact object's trajectory and the phase of the waveform. We present an evolution scheme for studying the effects of transient resonances and apply this to an astrophysically motivated population. We find that a large proportion of systems encounter a low-order resonance in the later stages of inspiral; however, the resulting effect on signal-to-noise recovery is small as a consequence of the low eccentricity of the inspirals. Neglecting the effects of transient resonances leads to a loss of 4% of detectable signals.Comment: 24 pages, 12 figures, 2 appendices; changes to match published versio

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Section: Discussionmentioning

confidence: 99%

“…Typically, the first term is nonzero and this gives the familiar oscillation. On resonance, it is zero, leaving the next-order term to govern the behaviour [46,86]. Only once we have moved far enough away from resonance for the first term to dominate the second do we recapture the nonresonant behaviour.…”

Section: A Timescalesmentioning

confidence: 98%

Importance of transient resonances in extreme-mass-ratio inspirals

et al. 2016

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“…FH show that for "most" orbits, G are not rapidly oscillating, and can significantly modify how the integrals of motion evolve during an inspiral. A given binary is very likely to evolve through several low-order resonances en route to the final merger of the smaller body with the large black hole [13]. A complete quantitative understanding of these resonant effects will thus be quite important for making accurate inspiral models.…”

Section: B Resonant Effectsmentioning

confidence: 99%

Resonantly enhanced and diminished strong-field gravitational-wave fluxes

Flanagan

Hughes

Ruangsri³

2014

Phys. Rev. D

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113

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The inspiral of a stellar mass (1 − 100 M⊙) compact body into a massive (10 5 − 10 7 M⊙) black hole has been a focus of much effort, both for the promise of such systems as astrophysical sources of gravitational waves, and because they are a clean limit of the general relativistic two-body problem. Our understanding of this problem has advanced significantly in recent years, with much progress in modeling the "self force" arising from the small body's interaction with its own spacetime deformation. Recent work has shown that this self interaction is especially interesting when the frequencies associated with the orbit's θ and r motions are in an integer ratio: Ω θ /Ωr = β θ /βr, with β θ and βr both integers. In this paper, we show that key aspects of the self interaction for such "resonant" orbits can be understood with a relatively simple Teukolsky-equation-based calculation of gravitational-wave fluxes. We show that fluxes from resonant orbits depend on the relative phase of radial and angular motions. The purpose of this paper is to illustrate in simple terms how this phase dependence arises using tools that are good for strong-field orbits, and to present a first study of how strongly the fluxes vary as a function of this phase and other orbital parameters. Future work will use the full dissipative self force to examine resonant and near resonant strong-field effects in greater depth, which will be needed to characterize how a binary evolves through orbital resonances.

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“…Consider a set of astrophysical inspirals with parameters such that they are likely to be important sources for lowfrequency GW detector. We have shown 11 that every inspiral will pass through at least one dynamically significant low-order resonance as it spirals through the detector's sensitive band. Many of these inspirals will pass through two significant resonances; some will pass through three.…”

Section: Adiabaticity and Its Limitations: Resonant Orbitsmentioning

confidence: 99%

Adiabatic and post-adiabatic approaches to extreme mass ratio inspiral

Hughes¹

2017

The Fourteenth Marcel Grossmann Meeting

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Extreme mass ratio inspirals (EMRIs) show a strong separation of timescales, with the time characterizing inspiral, T i , much longer than any time To characterizing orbital motions. The ratio of these timescales (which is essentially an EMRI's mass ratio) can be regarded as a parameter that controls a perturbative expansion. Here we describe the value and limitations of an "adiabatic" description of these binaries, which uses only the leading terms arising from such a two-timescale expansion. An adiabatic approach breaks down when orbits evolve through resonances, with important dynamical and observational consequences. We describe the shortfalls of an approach that only includes the adiabatic contributions to EMRI evolution, and outline what must be done to evolve these systems through resonance and to improve our ability to model EMRI systems more generally.Keywords: Black holes; black hole perturbation theory; gravitational waves. Motivation: The large-mass ratio limit of the two-body problem and extreme mass ratio inspiralsBinary systems in which one body is much more massive than the other can be analyzed perturbatively. We can describe such a binary as an exact black hole solution of general relativity (corresponding to the larger member of the binary) plus a correction due to the smaller body. Because the perturbation equations are much simpler to solve than the complete equations of general relativity, this turns out to be a limit that can be modeled very accurately and precisely. At least two major science goals drive studies of large mass ratio systems. First, these binaries represent a limit of the two-body problem that can be solved with high precision. As such, the study of these binaries provides important input to programs to solve the two-body problem of general relativity more generally, such as numerical relativity and the effective one-body approach 1-3 . Second, astrophysical extreme mass ratio inspirals (EMRIs) are expected to be important sources for space-based GW detectors such as eLISA 4 and DECIGO 5 . In this article, we will focus on the role of EMRIs as sources of gravitational waves (GWs). Such binaries are created when multibody interactions scatter stellar mass compact objects onto a strong-field, relativistic orbit of the black hole in a galaxy's center. Further evolution is then driven by GW emission. If the black hole has a mass of around 10 5 − 10 7 M , then these are targets for a detector like eLISA. The GWs that they generate can be heard out to z ∼ 0.5 − 1; we expect dozens to hundreds of events over a space-based detector's mission lifetime 6 . Measuring the GWs from these events will provide precision data on the characteristics of the large black hole, on the small body's orbit, and on the mass of the small bodyin short, a precision probe of the astrophysical population of galactic center black

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Census of transient orbital resonances encountered during binary inspiral

Cited by 48 publications

References 30 publications

Importance of transient resonances in extreme-mass-ratio inspirals

Importance of transient resonances in extreme-mass-ratio inspirals

Resonantly enhanced and diminished strong-field gravitational-wave fluxes

Adiabatic and post-adiabatic approaches to extreme mass ratio inspiral

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