Adiabatic equatorial inspirals of a spinning body into a Kerr black hole

Skoupý, Viktor; Lukes-Gerakopoulos, Georgios

doi:10.1103/physrevd.105.084033

Cited by 18 publications

(8 citation statements)

References 40 publications

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“…A generic EMRIs is in fact imagined to be an eccentric binary where both objects are spinning and the spins are not aligned with the orbital angular momentum. More specifically also the spin of the object with the smaller mass (usually called the secondary) is important and cannot be neglected [12][13][14][15][16].…”

Section: Introductionmentioning

confidence: 99%

Towards a gravitational self force-informed effective-one-body waveform model for nonprecessing, eccentric, large-mass-ratio inspirals

Nagar¹,

Albanesi²

2022

Preprint

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Building upon several recent advances in the development of effective-one-body models for spinaligned eccentric binaries with individual masses (m1, m2) we introduce a new EOB waveform model that aims at describing inspiralling binaries in the large mass-ratio regime, m1 m2. The model exploits the current state-of-the-art TEOBResumS-DALI model for eccentric binaries, but the standard EOB potentials (A, D, Q), informed by Numerical Relativity (NR) simulations, are replaced with the corresponding functions that are linear in the symmetric mass ratio ν ≡ m1m2/(m1 + m2) 2 taken at 8.5PN accuracy. To improve their strong-field behavior, these functions are: (i) suitably factorized and resummed using Padé approximants and (ii) additionally effectively informed to state-of-the-art numerical results obtained by gravitational self-force theory (GSF). For simplicity, the spin-sector of the model is taken to be the one of TEOBResumS-DALI, though removing the NR-informed spinorbit effective corrections. We propose the current GSF-informed EOB framework as a conceptually complete analytical tool to generate waveforms for eccentric Extreme (and Intermediate) Mass Ratio Inspirals for future gravitational wave detectors.

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Section: Introductionmentioning

confidence: 99%

Towards a gravitational self force-informed effective-one-body waveform model for nonprecessing, eccentric, large-mass-ratio inspirals

Nagar¹,

Albanesi²

2022

Preprint

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“…To calculate the fluxes we used a grid and Chebyshev interpolation like in [24]. In particular, we created a 10×4×3 grid in the (p, e, x) space for a = 0.5 (see Fig.…”

Section: Flux Gridmentioning

confidence: 99%

“…7) with the interpolation points located at the Chebyshev nodes. Note that the grid is simpler than in [24] since we do not come very close to the separatrix. The relative error of the Chebyshev interpolation is of the order 10 −3 which is similar to the relative errors of the fluxes themselves.…”

Section: Flux Gridmentioning

confidence: 99%

“…Combining these two perturbation theories we suggest in this work a scheme for adiabatic modelling of EMRIs aiming to contribute in the ongoing effort for more and more computationally efficient schemes [22,23]. The framework that we setup in this work could be expanded to other directions by adding more perturbative sources, like matter distribution around a black hole, [17] or the extended body effects induced by the secondary body [24].…”

Section: Introductionmentioning

confidence: 99%

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Action-Angle formalism for extreme mass ratio inspirals in Kerr spacetime

Kerachian¹,

Polcar²,

Skoupý³

et al. 2023

Preprint

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We introduce an action-angle formalism for bounded geodesic motion in Kerr black hole spacetime using canonical perturbation theory. Namely, we employ a Lie series technique to produce a series of canonical transformations on a Hamiltonian function describing geodesic motion in Kerr background written in Boyer-Lindquist coordinates to a Hamiltonian system written in action-angle variables. This technique allows us to produce a closed-form invertible relation between the Boyer-Lindquist variables and the action-angle ones, while it generates in analytical closed form all the characteristic functions of the system as well. The expressed in the action-angle variable Hamiltonian system is employed to model an extreme mass ratio inspiral (EMRI), i.e. a binary system where a stellar compact object inspirals into a supermassive black hole due to gravitational radiation reaction. We consider the adiabatic evolution of an EMRI, for which the energy and angular momentum fluxes are computed by solving the Teukolsky equation in the frequency domain. To achieve this a new Teukolsky equation solver code was developed.

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“…We will further accelerate our model toward EMRI data analysis, using the efficiencyoriented FASTEMRIWAVEFORMS framework [100], which will enable a highly parallelized implementation with graphics processing units [64,67]. Ultimately, we will work on refining the adiabatic model by combining analytical PN-GSF results with numerical GSF data [26][27][28]63,65,[157][158][159][160][161][162][163] to accomplish a science-adequate, postadiabatic waveform for LISA.…”

Section: If We Write I Oscmentioning

confidence: 99%