Effective-one-body Hamiltonian with next-to-leading order spin-spin coupling for two nonprecessing black holes with aligned spins

Balmelli, Simone; Jetzer, Philippe

doi:10.1103/physrevd.87.124036

Cited by 24 publications

(13 citation statements)

References 50 publications

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“…Identifying the various powers of u andâ on both sides of Eq. (2.22) allows one to convert our analytical results (3.10)-(3.11) into an analytical knowledge of the PN expansions of f (n)resc A (u) and δG (n)resc S (u) (with n = 0, 2), with the following results: The only terms among the above, high-accuracy, PN expansions that were known from standard PN compu-tations were the next-to-leading-order (NLO) corrections to δG (0)resc S (i.e., 1 + 102 5 u) [57,58] and to f (0)resc A (u) (i.e., 1 + 11 4 u) [59].…”

Section: Analytical Computation Of the Self-force Corrections To mentioning

confidence: 99%

Spin-dependent two-body interactions from gravitational self-force computations

2015

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We analytically compute, through the eight-and-a-half post-Newtonian order and the fourth-order in spin, the gravitational self-force correction to Detweiler's gauge invariant redshift function for a small mass in circular orbit around a Kerr black hole. Using the first law of mechanics for black hole binaries with spin [L. Blanchet, A. Buonanno and A. Le Tiec, Phys. Rev. D 87, 024030 (2013)] we transcribe our results into a knowledge of various spin-dependent couplings, as encoded within the spinning effective-one-body model of T. Damour and A. Nagar [Phys. Rev. D 90, 044018 (2014)]. We also compare our analytical results to the (corrected) numerical self-force results of A. G. Shah, J. L. Friedman and T. S. Keidl [Phys. Rev. D 86, 084059 (2012)], from which we show how to directly extract physically relevant spin-dependent couplings.

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Section: Analytical Computation Of the Self-force Corrections To mentioning

confidence: 99%

Spin-dependent two-body interactions from gravitational self-force computations

2015

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“…[33,[45][46][47]94,134,412,414,415,513,514], and one by T. Damour, A. Nagar, and their collaborators, e.g. [40,70,143,149,150,154,158,158,159,[161][162][163]381,391,393,396,398,399]. These BBH EOB models both reproduce the PN and test-mass results in the appropriate limits, use the same energy mapping to the effective phase spaces, and the effective description of a test particle in an effective spacetime.…”

Section: Tidal Effective-one-body Models For Binary Inspiralsmentioning

confidence: 91%

Interpreting binary neutron star mergers: describing the binary neutron star dynamics, modelling gravitational waveforms, and analyzing detections

2021

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Gravitational waves emitted from the coalescence of neutron star binaries open a new window to probe matter and fundamental physics in unexplored, extreme regimes. To extract information about the supranuclear matter inside neutron stars and the properties of the compact binary systems, robust theoretical prescriptions are required. We give an overview about general features of the dynamics and the gravitational wave signal during the binary neutron star coalescence. We briefly describe existing analytical and numerical approaches to investigate the highly dynamical, strong-field region during the merger. We review existing waveform approximants and discuss properties and possible advantages and shortcomings of individual waveform models, and their application for real gravitational-wave data analysis.

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“…The chirping signals emitted by inspiraling binaries contain a range of frequency components: if the graviton has mass, the components propagate at different speeds, again given by Eq. (44). This effect can be modeled in the templates used to search for binary signals by including a λ g dependence in the waveform phasing [470].…”

Section: Tests Of Gravitational-wave Propagationmentioning

confidence: 99%

Testing General Relativity with Low-Frequency, Space-Based Gravitational-Wave Detectors

Gair¹,

Vallisneri

Larson

et al. 2013

Living Rev. Relativ.

312

310

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We review the tests of general relativity that will become possible with space-based gravitational-wave detectors operating in the ∼ 10−5 − 1 Hz low-frequency band. The fundamental aspects of gravitation that can be tested include the presence of additional gravitational fields other than the metric; the number and tensorial nature of gravitational-wave polarization states; the velocity of propagation of gravitational waves; the binding energy and gravitational-wave radiation of binaries, and therefore the time evolution of binary inspirals; the strength and shape of the waves emitted from binary mergers and ringdowns; the true nature of astrophysical black holes; and much more. The strength of this science alone calls for the swift implementation of a space-based detector; the remarkable richness of astrophysics, astronomy, and cosmology in the low-frequency gravitational-wave band make the case even stronger.

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Effective-one-body Hamiltonian with next-to-leading order spin-spin coupling for two nonprecessing black holes with aligned spins

Cited by 24 publications

References 50 publications

Spin-dependent two-body interactions from gravitational self-force computations

Spin-dependent two-body interactions from gravitational self-force computations

Interpreting binary neutron star mergers: describing the binary neutron star dynamics, modelling gravitational waveforms, and analyzing detections

Testing General Relativity with Low-Frequency, Space-Based Gravitational-Wave Detectors

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