Evolution of small-mass-ratio binaries with a spinning secondary

Warburton, Niels; Osburn, Thomas; Evans, Charles R.

doi:10.1103/physrevd.96.084057

Cited by 67 publications

(67 citation statements)

References 124 publications

(203 reference statements)

Supporting

Mentioning

Contrasting

Order By: Relevance

“…(vi) The results of this work should be incorporated into practical inspiral evolution schemes. The conservative effects from a spinning secondary have been examined [80,81], but as yet, the influence of the dissipative spin effects remains to be explored.…”

Section: Discussionmentioning

confidence: 99%

Dissipation in extreme mass-ratio binaries with a spinning secondary

et al. 2020

Self Cite

View full text Add to dashboard Cite

We present the gravitational-wave flux balance law in an extreme mass-ratio binary with a spinning secondary. This law relates the flux of energy (angular momentum) radiated to null infinity and through the event horizon to the local change in the secondary's orbital energy (angular momentum) for generic (non-resonant) bound orbits in Kerr spacetime. As an explicit example we compute these quantities for a spin-aligned body moving on a circular orbit around a Schwarzschild black hole. We perform this calculation both analytically, via a high-order post-Newtonian expansion, and numerically in two different gauges. Using these results we demonstrate explicitly that our new balance law holds. I. INTRODUCTION Gravitational wave physics is now firmly established as an observational science. Ground-based detectors regularly observe the binary mergers of stellar-mass black holes and neutron stars [1]. Looking to the future, the construction of the space-based millihertz detector, LISA [2], will open a new window on binaries with a total mass in the range 10 4-10 7 M. One particularly interesting class of such systems are extreme mass-ratio inspirals (EMRIs) [3]. In these binaries, a compact object, such as a stellar mass black hole or neutron star, spirals into a massive black hole driven by the emission of gravitational waves. These systems have a (small) mass-ratio in the range of 10 −4 − 10 −7. In general EMRIs are not expected to completely circularize by the time of merger, resulting in a rich orbital and waveform structure that carries with it detailed information about the spacetime of the EMRI [4]. Additional complexity is added by the expectation that both the primary (larger) and secondary (smaller) compact object will be spinning, with no preferred alignment between the secondary's spin and the orbital angular momentum. Modelling the effects of the spin of the secondary is the focus of the present work. Extracting EMRI signals from the LISA data stream will require precise theoretical waveform models of these binaries. This is because the instantaneous signal-to-noise ratio of a typical EMRI will be very small, and so the waveforms can only be separated from the instrumental noise and the potentially many other competing sources by semi-coherent matched filtering techniques [3]. The small mass ratio in EMRIs naturally suggests black hole perturbation theory as a modelling approach. With this method, the spacetime of the binary is expanded around the analytically-known spacetime of the primary. The leading order contribution to the waveform phase comes from the orbit-averaged fluxes of gravitational radiation. These were calculated for a non-spinning secondary moving along a circular orbit about Kerr black hole in the 1970's [5]. These calculations were extended to eccentric [6] and fully generic (inclined) motion [7-9] in the 2000's. The waveforms that can be constructed from these results will likely be sufficient for detection of the very loudest EMRIs. In order to detect the many weaker signals, to perform...

show abstract

Section: Discussionmentioning

confidence: 99%

Dissipation in extreme mass-ratio binaries with a spinning secondary

et al. 2020

Self Cite

View full text Add to dashboard Cite

show abstract

“…Finally, concrete computations of EMRIs with spin effects were carried out in Refs. [23][24][25][26][27].…”

Section: Introductionmentioning

confidence: 99%

Hamilton-Jacobi equation for spinning particles near black holes

Witzany

2019

Phys. Rev. D

View full text Add to dashboard Cite

A compact stellar-mass object inspiralling onto a massive black hole deviates from geodesic motion due to radiation-reaction forces as well as finite-size effects. Such post-geodesic deviations need to be included with sufficient precision into wave-form models for the upcoming space-based gravitational-wave detector LISA. I present the formulation and solution of the Hamilton-Jacobi equation of geodesics near Kerr black holes perturbed by the so-called spin-curvature coupling, the leading order finite-size effect. In return, this solution allows to compute a number of observables such as the turning points of the orbits as well as the fundamental frequencies of motion. This result provides one of the necessary ingredients for waveform models for LISA and an important contribution useful for the relativistic two-body problem in general.

show abstract

“…Currently, at first order it is possible to simulate full inspirals, driven by the first-order self-force, from a spinning small object on a generic orbit in a Schwarzschild background [14][15][16][17] or the adiabatic inspiral of an object in the equatorial plane of a Kerr black hole [18]. While no analogous inspirals have yet been computed for generic, inclined orbits in Kerr, it is also now possible to calculate the first-order self-force on any fixed bound orbit in Kerr [19].…”

Section: A Second-order Gravitational Self-forcementioning

confidence: 99%

Second-order gravitational self-force in a highly regular gauge

Upton

Pound

2021

Phys. Rev. D

View full text Add to dashboard Cite

Extreme-mass-ratio inspirals (EMRIs) will be key sources for LISA. However, accurately extracting system parameters from a detected EMRI waveform will require self-force calculations at second order in perturbation theory, which are still in a nascent stage. One major obstacle in these calculations is the strong divergences that are encountered on the worldline of the small object. Previously, it was shown by one of us [Phys. Rev. D 95, 104056 (2017)] that a class of "highly regular" gauges exist in which the singularities have a qualitatively milder form, promising to enable more efficient numerical calculations. Here we derive expressions for the metric perturbation in this class of gauges, in a local expansion in powers of distance r from the worldline, to sufficient order in r for numerical implementation in a puncture scheme. Additionally, we use the highly regular class to rigorously derive a distributional source for the second-order field and a pointlike second-order stress-energy tensor (the Detweiler stress-energy) for the small object. This makes it possible to calculate the second-order self-force using mode-sum regularisation rather than the more cumbersome puncture schemes that have been necessary previously. Although motivated by EMRIs, our calculations are valid in an arbitrary vacuum background, and they may help clarify the interpretation of point masses and skeleton sources in general relativity more broadly.

show abstract

Evolution of small-mass-ratio binaries with a spinning secondary

Cited by 67 publications

References 124 publications

Dissipation in extreme mass-ratio binaries with a spinning secondary

Dissipation in extreme mass-ratio binaries with a spinning secondary

Hamilton-Jacobi equation for spinning particles near black holes

Second-order gravitational self-force in a highly regular gauge

Contact Info

Product

Resources

About