Geodesic Models of Quasi-periodic-oscillations as Probes of Quadratic Gravity

Maselli, Andrea; Pani, Paolo; Cotesta, R.; Gualtieri, Leonardo; Ferrari, Valeria; Stella, L.

doi:10.3847/1538-4357/aa72e2

Cited by 61 publications

(60 citation statements)

References 54 publications

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“…For example, the orbital plane of test particles, if not aligned with the equatorial plane, will precess around the angular momentum axis of the rotating body, the Lense-Thirring effect [19]. We can investigate this phenomenon studying the precession frequencies Ω r and Ω θ , which describe the perturbation in circular orbits due r and θ velocity components [20,21] (analytic expressions for these quantities can be found in the supplementary material). The BH quadrupole moment is [22] Q 20 = − 64π 15…”

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confidence: 99%

Black Holes in an Effective Field Theory Extension of General Relativity

et al. 2018

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Effective field theory methods suggest that some rather-general extensions of General Relativity include, or are mimicked by, certain higher-order curvature corrections, with coupling constants expected to be small but otherwise arbitrary. Thus, the tantalizing prospect to test the fundamental nature of gravity with gravitational-wave observations, in a systematic way, emerges naturally. Here, we build black hole solutions in such a framework and study their main properties. Once rotation is included, we find the first purely gravitational example of geometries without Z2-symmetry. Despite the higher-order operators of the theory, we show that linearized fluctuations of such geometries obey second-order differential equations. We find nonzero tidal Love numbers. We study and compute the quasinormal modes of such geometries. These results are of interest to gravitational-wave science but also potentially relevant for electromagnetic observations of the galactic center or X-ray binaries.

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confidence: 99%

Black Holes in an Effective Field Theory Extension of General Relativity

et al. 2018

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“…• p = 4: this case includes Einstein-scalar-Gauss-Bonnet [49,52,[84][85][86] and dynamical Chern-Simons gravity [51,87,88]. In this case…”

Section: A Special Casesmentioning

confidence: 99%

Parametrized ringdown spin expansion coefficients: A data-analysis framework for black-hole spectroscopy with multiple events

et al. 2020

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Black-hole spectroscopy is arguably the most promising tool to test gravity in extreme regimes and to probe the ultimate nature of black holes with unparalleled precision. These tests are currently limited by the lack of a ringdown parametrization that is both robust and accurate. We develop an observable-based parametrization of the ringdown of spinning black holes beyond general relativity, which we dub ParSpec (Parametrized Ringdown Spin Expansion Coefficients). This approach is perturbative in the spin, but it can be made arbitrarily precise (at least in principle) through a high-order expansion. It requires O(10) ringdown detections, which should be routinely available with the planned space mission LISA and with third-generation ground-based detectors. We provide a preliminary analysis of the projected bounds on parametrized ringdown parameters with LISA and with the Einstein Telescope, and discuss extensions of our model that can be straightforwardly included in the future. arXiv:1910.12893v1 [gr-qc] 28 Oct 2019where J = 1, 2, ..., q labels the mode; M i and χ i 1 are the detector-frame mass and spin of the i-th source, both measured assuming GR (see below); D is the order of the spin expansion; w (n) J and t (n) J are the dimensionless coefficients of the spin expansion for a Kerr BH in GR (provided in Table I for a few representative modes); γ i are dimensionless coupling constants, which can depend on the source i -see Eq. (6) below -but do not depend 1 The QNMs are identified by three integer numbers: the angular momentum number l, the azimuthal number m ∈ [−l, l], and the overtone number, which we set to zero in this paper, i.e. we only consider fundamental modes. For ease of notation we leave these indices implicit, i.e. ω (J) ≡ ω (0lm) , where J is an index that labels the mode. (n) J and δt (n) J (n) J and δt (n) J (or, equivalently, δW (n) J and δT (n) J ), these corrections depend only on the theory and not on the source.It is easy to check that, to leading order in α, the redefinitionsbring Eqs. (A1) and (A2) to the form in Eqs.(3) and (4) used in the main text. The above redefinitions also show that there is some degeneracy among the beyond-GR parameters, and that one can only constrain the combinations δw (n) J and δt (n) J , which contains the intrinsic mode corrections (δW (n) J and δT (n) J ) and the mass and spin corrections (δm and δχ).(n) J and δt (n) J are unconstrained by the data.

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“…Another avenue for future work includes improving the analysis for bounding dCS gravity from BH-PSR observations. In this paper, we used the stellar mass BH quadrupole moment obtained within the slow-rotation approximation [61,62] for BH-PSR systems with the BH dimensionless spin of unity, and thus the bounds should only be understood as order of magnitude estimates. One could improve this analysis by deriving the BH quadrupole moment valid for arbitrary spin.…”

Section: Conclusion and Discussionmentioning

confidence: 99%

“…Analytic BH solutions with arbitrary spin in these theories have not been found yet. Non-rotating and slowly-rotating analytic BH solutions have been constructed in [54][55][56][57][58] for EdGB and in [59][60][61][62] for dCS.…”

Section: Introductionmentioning

confidence: 99%

Testing general relativity with black hole-pulsar binaries

Seymour

Yagi

2018

Phys. Rev. D

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Binary pulsars allow us to carry out precision tests of gravity and have placed stringent bounds on a broad class of theories beyond general relativity. Current and future radio telescopes, such as FAST, SKA, and MeerKAT, may find a new astrophysical system, a pulsar orbiting around a black hole, which will provide us a new source for probing gravity. In this paper, we systematically study the prospects of testing general relativity with such black hole-pulsar binaries. We begin by finding a mapping between generic non-Einsteinian parameters in the orbital decay rate and theoretical constants in various modified theories of gravity and then summarize this mapping with a ready-to-use list. Theories we study here include scalar-tensor theories, varying G theories, massive gravity theories, generic screening gravity and quadratic curvature-corrected theories. We next use simulated measurement accuracy of the orbital decay rate for black hole-pulsar binaries with FAST/SKA and derive projected upper bounds on the above generic non-Einsteinian parameters. We find that such bounds from black hole-pulsars can be stronger than those from neutron starpulsar and neutron star-white dwarf binaries by a few orders of magnitude when the correction enters at negative post-Newtonian orders. By mapping such bounds on generic parameters to those on various modified theories of gravity, we find that one can constrain the amount of time variation in Newton's constant G to be comparable to or slightly weaker than than the current strongest bound from solar system experiments, though the former bounds are complementary to the latter since they probe different regime of gravity. We also study how well one can probe quadratic gravity from black hole quadrupole moment measurements of black hole-pulsars. We find that bounds on the parity-violating sector of quadratic gravity can be stronger than current bounds by six orders of magnitude. These results suggest that a new discovery of black hole-pulsars in the future will provide powerful ways to probe gravity further.

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Geodesic Models of Quasi-periodic-oscillations as Probes of Quadratic Gravity

Cited by 61 publications

References 54 publications

Black Holes in an Effective Field Theory Extension of General Relativity

Black Holes in an Effective Field Theory Extension of General Relativity

Parametrized ringdown spin expansion coefficients: A data-analysis framework for black-hole spectroscopy with multiple events

Testing general relativity with black hole-pulsar binaries

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