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438 results on '"alternative theories of gravity"'

151. Tests of general relativity with stellar-mass black hole binaries observed by LISA

Author

Enrico Barausse, Stanislav Babak, Alexandre Toubiana, Sylvain Marsat, John G. Baker, AstroParticule et Cosmologie (APC (UMR_7164)), Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Observatoire de Paris, Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Centre National de la Recherche Scientifique (CNRS)-Université de Paris (UP), Institut d'Astrophysique de Paris (IAP), Institut national des sciences de l'Univers (INSU - CNRS)-Sorbonne Université (SU)-Centre National de la Recherche Scientifique (CNRS), and Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Centre National de la Recherche Scientifique (CNRS)-Université Paris Cité (UPCité)

Subjects
Stellar mass, General relativity, FOS: Physical sciences, alternative theories of gravity, General Relativity and Quantum Cosmology (gr-qc), graviton: mass, 01 natural sciences, General Relativity and Quantum Cosmology, Monte Carlo: Markov chain, Gravitation, Theoretical physics, Settore FIS/05 - Astronomia e Astrofisica, binary: coalescence, statistical analysis, Tests of general relativity, 0103 physical sciences, Equivalence principle, 010306 general physics, gravitation: dipole, radiation: dipole, Physics, astro-ph.HE, High Energy Astrophysical Phenomena (astro-ph.HE), LISA, 010308 nuclear & particles physics, Gravitational wave, Graviton, gravitational radiation, statistical analysis: Bayesian, black hole: mass, Black hole, detector: sensitivity, frequency: low, equivalence principle, black hole: binary, gravitational radiation: emission, graviton, [PHYS.GRQC]Physics [physics]/General Relativity and Quantum Cosmology [gr-qc], Astrophysics - High Energy Astrophysical Phenomena, [PHYS.ASTR]Physics [physics]/Astrophysics [astro-ph]
Abstract

We consider the observation of stellar-mass black holes binaries with the Laser Interferometer Space Antenna (LISA). Preliminary results based on Fisher information matrix analyses have suggested that gravitational waves from those sources could be very sensitive to possible deviations from the theory of general relativity and from the strong equivalence principle during the low-frequency binary inspiral. We perform a full Markov Chain Monte Carlo Bayesian analysis to quantify the sensitivity of these signals to two phenomenological modifications of general relativity, namely a putative gravitational dipole emission and a non-zero mass for the graviton, properly accounting for the detector's response. Moreover, we consider a scenario where those sources could be observed also with Earth-based detectors, which should measure the coalescence time with precision better than $1 \ {\rm ms}$. This constraint on the coalescence time further improves the bounds that we can set on those phenomenological deviations from general relativity. We show that tests of dipole radiation and the graviton's mass should improve respectively by seven and half an order(s) of magnitude over current bounds. Finally, we discuss under which conditions one may claim the detection of a modification to general relativity., Comment: Update references

Published
2020
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152. Black holes in torsion bigravity

Author

Vasilisa Nikiforova, Thibault Damour, Institut des Hautes Etudes Scientifiques (IHES), and IHES

Subjects
Physics, 010308 nuclear & particles physics, Astrophysics::High Energy Astrophysical Phenomena, FOS: Physical sciences, alternative theories of gravity, General Relativity and Quantum Cosmology (gr-qc), Parameter space, 16. Peace & justice, 01 natural sciences, General Relativity and Quantum Cosmology, Black hole, Massless particle, symbols.namesake, Theoretical physics, Bimetric gravity, General relativity, 0103 physical sciences, Torsion (algebra), Schwarzschild metric, symbols, [PHYS.GRQC]Physics [physics]/General Relativity and Quantum Cosmology [gr-qc], Einstein, Connection (algebraic framework), 010306 general physics
Abstract

We study spherically symmetric black hole solutions in a four-parameter Einstein-Cartan-type class of theories, called "torsion bigravity". These theories offer a geometric framework (with a metric and an independent torsionfull connection) for a modification of Einstein's theory that has the same spectrum as bimetric gravity models. In addition to an Einsteinlike massless spin-2 excitation, there is a massive spin-2 one (of range $\kappa^{-1}$) coming from the torsion sector, rather than from a second metric. We prove the existence of three broad classes of spherically-symmetric black hole solutions in torsion bigravity. First, the Schwarzschild solution defines an asymptotically-flat torsionless black hole for all values of the parameters. [And we prove that one cannot deform a Schwarzschild solution, at the linearized level, by adding an infinitesimal torsion hair.] Second, when considering finite values of the range, we find that there exist non-asymptotically-flat torsion-hairy black holes in a large domain of parameter space. Third, we find that, in the limit of infinite range, there exists a two-parameter family of asymptotically flat torsion-hairy black holes. The latter black hole solutions give an interesting example of non-Einsteinian (but still purely geometric) black hole structures which might be astrophysically relevant when considering a range of cosmological size., Comment: 19 pages, 3 figures

Published
2020
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153. Absence of a Vainshtein radius in torsion bigravity

Author

Vasilisa Nikiforova, Institut des Hautes Etudes Scientifiques (IHES), and IHES

Subjects
High Energy Physics - Theory, perturbation, Inverse, FOS: Physical sciences, alternative theories of gravity, General Relativity and Quantum Cosmology (gr-qc), 01 natural sciences, General Relativity and Quantum Cosmology, weak field, Bimetric gravity, 0103 physical sciences, excited state, symmetry: rotation, 010306 general physics, Scaling, Einstein-Cartan, Mathematical physics, Ansatz, Physics, 010308 nuclear & particles physics, [PHYS.HTHE]Physics [physics]/High Energy Physics - Theory [hep-th], scaling, Torsion (mechanics), torsion, Vainshtein, Massless particle, Nonlinear system, High Energy Physics - Theory (hep-th), General relativity, [PHYS.GRQC]Physics [physics]/General Relativity and Quantum Cosmology [gr-qc], nonlinear, Excitation
Abstract

It was pointed out long ago by Vainshtein [Phys. Lett. 39B, 393 (1972)] that the weak-field perturbation expansion of generic theories (of the nonlinear Fierz-Pauli type) involving massive spin-2 excitations breaks down below a certain distance around a material source ("Vainshtein radius"), scaling as some inverse power of the spin-2 mass $m_2$, i.e., some positive power of the range $m_2^{-1}$. Here we prove that this conclusion does not apply in a generalized Einstein-Cartan theory (called "torsion bigravity") whose spectrum is made (like that of bimetric gravity) of a massless spin-2 excitation and a massive spin-2 one. Working within a static spherically symmetric ansatz, we prove, by reformulating the field equations in terms of new variables, that one can construct an all-order weak-field perturbative expansion where no denominators involving $m_2$ ever appear in the region $r \ll m_2^{-1}$. In particular, we show how the formal large-range limit, $m_2 \to 0$, leads to a well-defined, finite perturbation expansion, whose all-order structure is discussed in some detail., 18 pages, no figures

Published
2020
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154. Towards numerical relativity in scalar Gauss-Bonnet gravity: 3+1 decomposition beyond the small-coupling limit

Author

Helvi Witek, Paolo Pani, and Leonardo Gualtieri

Subjects
High Energy Physics - Theory, Coupling constant, Physics, 010308 nuclear & particles physics, General relativity, Scalar (mathematics), FOS: Physical sciences, alternative theories of gravity, General Relativity and Quantum Cosmology (gr-qc), numerical relativity, 16. Peace & justice, Curvature, 01 natural sciences, General Relativity and Quantum Cosmology, Numerical relativity, Theoretical physics, Quadratic equation, Theory of relativity, High Energy Physics - Theory (hep-th), gravitational waves, Gauss–Bonnet gravity, 0103 physical sciences, gravitational waves, numerical relativity, alternative theories of gravity, 010306 general physics
Abstract

Scalar Gauss-Bonnet gravity is the only theory with quadratic curvature corrections to general relativity whose field equations are of second differential order. This theory allows for nonperturbative dynamical corrections and is therefore one of the most compelling case studies for beyond-general relativity effects in the strong-curvature regime. However, having second-order field equations is not a guarantee for a healthy time evolution in generic configurations. As a first step towards evolving black-hole binaries in this theory, we here derive the 3+1 decomposition of the field equations for any (not necessarily small) coupling constant and we discuss potential challenges of its implementation., 8 pages

Published
2020

155. Gaussian processes for the interpolation and marginalization of waveform error in extreme-mass-ratio-inspiral parameter estimation

Author

Natalia Korsakova, Christopher J. Moore, Stanislav Babak, Jonathan R. Gair, A. J. K. Chua, Astrophysique Relativiste Théories Expériences Métrologie Instrumentation Signaux (ARTEMIS), Université Nice Sophia Antipolis (1965 - 2019) (UNS), COMUE Université Côte d'Azur (2015-2019) (COMUE UCA)-COMUE Université Côte d'Azur (2015-2019) (COMUE UCA)-Institut national des sciences de l'Univers (INSU - CNRS)-Observatoire de la Côte d'Azur, COMUE Université Côte d'Azur (2015-2019) (COMUE UCA)-Université Côte d'Azur (UCA)-Université Côte d'Azur (UCA)-Centre National de la Recherche Scientifique (CNRS), AstroParticule et Cosmologie (APC (UMR_7164)), Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Observatoire de Paris, Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Centre National de la Recherche Scientifique (CNRS)-Université Paris Cité (UPCité), Université Nice Sophia Antipolis (... - 2019) (UNS), Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Centre National de la Recherche Scientifique (CNRS)-Université de Paris (UP), Université Côte d'Azur (UCA)-Université Côte d'Azur (UCA)-Institut national des sciences de l'Univers (INSU - CNRS)-Observatoire de la Côte d'Azur, Université Côte d'Azur (UCA)-Centre National de la Recherche Scientifique (CNRS), Observatoire de Paris, PSL Research University (PSL)-PSL Research University (PSL)-Université Paris Diderot - Paris 7 (UPD7)-Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Centre National de la Recherche Scientifique (CNRS), Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Centre National de la Recherche Scientifique (CNRS)-Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Observatoire de Paris, and PSL Research University (PSL)-PSL Research University (PSL)-Université Paris Diderot - Paris 7 (UPD7)

Subjects
Systematic error, alternative theories of gravity, 01 natural sciences, symbols.namesake, binary: coalescence, 0103 physical sciences, numerical methods, Applied mathematics, Waveform, [PHYS.PHYS.PHYS-INS-DET]Physics [physics]/Physics [physics]/Instrumentation and Detectors [physics.ins-det], 010306 general physics, numerical calculations, Gaussian process, Physics, LISA, 010308 nuclear & particles physics, Estimation theory, gravitational radiation, Mass ratio, gravitational radiation detector, General relativity, gravitational radiation: emission, symbols, [PHYS.GRQC]Physics [physics]/General Relativity and Quantum Cosmology [gr-qc], [PHYS.ASTR]Physics [physics]/Astrophysics [astro-ph], Interpolation
Abstract

A number of open problems hinder our present ability to extract scientific information from data that will be gathered by the near-future gravitational-wave mission LISA. Many of these relate to the modeling, detection, and characterization of signals from binary inspirals with an extreme component-mass ratio of $\ensuremath{\lesssim}{10}^{\ensuremath{-}4}$. In this paper, we draw attention to the issue of systematic error in parameter estimation due to the use of fast but approximate waveform models; this is found to be relevant for extreme-mass-ratio inspirals even in the case of waveforms with $\ensuremath{\gtrsim}90%$ overlap accuracy and moderate ($\ensuremath{\gtrsim}30$) signal-to-noise ratios. A scheme that uses Gaussian processes to interpolate and marginalize over waveform error is adapted and investigated as a possible precursor solution to this problem. Several new methodological results are obtained, and the viability of the technique is successfully demonstrated on a three-parameter example in the setting of the LISA Data Challenge.

Published
2020
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156. Reflection-asymmetric wormholes and their double shadows

Author

Marek A. Abramowicz, Jiří Horák, Maciek Wielgus, Frederic Vincent, Laboratoire d'études spatiales et d'instrumentation en astrophysique (LESIA (UMR_8109)), Institut national des sciences de l'Univers (INSU - CNRS)-Observatoire de Paris, and Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Université Paris Diderot - Paris 7 (UPD7)-Sorbonne Université (SU)-Centre National de la Recherche Scientifique (CNRS)

Subjects
Photon, Observer (quantum physics), FOS: Physical sciences, alternative theories of gravity, Model parameters, General Relativity and Quantum Cosmology (gr-qc), 01 natural sciences, General Relativity and Quantum Cosmology, topological, Theoretical physics, 0103 physical sciences, black hole, symmetry: rotation, Wormhole, 010306 general physics, High Energy Astrophysical Phenomena (astro-ph.HE), Physics, Spacetime, 010308 nuclear & particles physics, photon, parametrization, space-time: Reissner-Nordstroem, General relativity, wormhole, [PHYS.GRQC]Physics [physics]/General Relativity and Quantum Cosmology [gr-qc], shadowing, Astrophysics - High Energy Astrophysical Phenomena, [PHYS.ASTR]Physics [physics]/Astrophysics [astro-ph], asymmetry
Abstract

We discuss construction and observational properties of wormholes obtained by connecting two Reissner-Nordstrom spacetimes with distinct mass and charge parameters. These objects are spherically symmetric, but not reflection-symmetric, as the connected spacetimes differ. The reflection-asymmetric wormholes may reflect a significant fraction of the infalling radiation back to the spacetime of its origin. We interpret this effect in a simple framework of the effective photon potential. Depending on the model parameters, image of such a wormhole seen by a distant observer (its "shadow") may contain a photon ring formed on the observer's side, photon ring formed on the other side of the wormhole, or both photon rings. These unique topological features would allow us to firmly distinguish this class of objects from Kerr black holes using radioastronomical observations., 9 pages, accepted in Phys. Rev. D

Published
2020
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157. Frequency domain reduced order model of aligned-spin effective-one-body waveforms with higher-order modes

Author

Sylvain Marsat, M. Pürrer, R. Cotesta, AstroParticule et Cosmologie (APC (UMR_7164)), Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Observatoire de Paris, Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Centre National de la Recherche Scientifique (CNRS)-Université de Paris (UP), and Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Centre National de la Recherche Scientifique (CNRS)-Université Paris Cité (UPCité)

Subjects
data analysis method, higher-order, Binary number, FOS: Physical sciences, alternative theories of gravity, General Relativity and Quantum Cosmology (gr-qc), 01 natural sciences, Bayesian, General Relativity and Quantum Cosmology, Binary black hole, 0103 physical sciences, numerical methods, Waveform, 010306 general physics, numerical calculations, Physics, [PHYS]Physics [physics], 010308 nuclear & particles physics, Estimation theory, Mathematical analysis, Spherical harmonics, Order (ring theory), black hole: binary, General relativity, relativity theory, Frequency domain, gravitational radiation: emission, [PHYS.GRQC]Physics [physics]/General Relativity and Quantum Cosmology [gr-qc], [PHYS.ASTR]Physics [physics]/Astrophysics [astro-ph], Order of magnitude, asymmetry
Abstract

We present a frequency domain reduced order model (ROM) for the aligned-spin effective-one-body (EOB) model for binary black holes (BBHs) SEOBNRv4HM that includes the spherical harmonics modes $(\ell, |m|) = (2,1),(3,3),(4,4),(5,5)$ beyond the dominant $(\ell, |m|) = (2,2)$ mode. These higher modes are crucial to accurately represent the waveform emitted from asymmetric BBHs. We discuss a decomposition of the waveform, extending other methods in the literature, that allows us to accurately and efficiently capture the morphology of higher mode waveforms. We show that the ROM is very accurate with median (maximum) values of the unfaithfulness against SEOBNRv4HM lower than $0.001\% (0.03\%)$ for total masses in $[2.8,100] M_\odot$. For a total mass of $M = 300 M_\odot$ the median (maximum) value of the unfaithfulness increases up to $0.004\% (0.17\%)$. This is still at least an order of magnitude lower than the estimated accuracy of SEOBNRv4HM compared to numerical relativity simulations. The ROM is two orders of magnitude faster in generating a waveform compared to SEOBNRv4HM. Data analysis applications typically require $\mathcal{O}(10^6-10^8)$ waveform evaluations for which SEOBNRv4HM is in general too slow. The ROM is therefore crucial to allow the SEOBNRv4HM waveform to be used in searches and Bayesian parameter inference. We present a targeted parameter estimation study that shows the improvements in measuring binary parameters when using waveforms that includes higher modes and compare against three other waveform models., Fix label in Fig.10

Published
2020
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158. Sixth post-Newtonian local-in-time dynamics of binary systems

Author

Thibault Damour, Andrea Geralico, Donato Bini, Institut des Hautes Etudes Scientifiques (IHES), and IHES

Subjects
Physics, Simplex, 010308 nuclear & particles physics, Delaunay triangulation, Scattering, Computation, Binary number, FOS: Physical sciences, alternative theories of gravity, General Relativity and Quantum Cosmology (gr-qc), Mass ratio, 01 natural sciences, General Relativity and Quantum Cosmology, Gravitation, symbols.namesake, 6 Post-Newtonian approximation, General relativity, 0103 physical sciences, symbols, [PHYS.GRQC]Physics [physics]/General Relativity and Quantum Cosmology [gr-qc], Two-body system Hamiltonian, 010306 general physics, Hamiltonian (quantum mechanics), Mathematical physics
Abstract

Using a recently introduced method [Phys.\ Rev.\ Lett.\ {\bf 123}, 231104 (2019)], which splits the conservative dynamics of gravitationally interacting binary systems into a non-local-in-time part and a local-in-time one, we compute the local part of the dynamics at the sixth post-Newtonian (6PN) accuracy. Our strategy combines several theoretical formalisms: post-Newtonian, post-Minkowskian, multipolar-post-Minkowskian, effective-field-theory, gravitational self-force, effective one-body, and Delaunay averaging. The full functional structure of the local 6PN Hamiltonian (which involves 151 numerical coefficients) is derived, but contains four undetermined numerical coefficients. Our 6PN-accurate results are complete at orders $G^3$ and $G^4$, and the derived $O(G^3)$ scattering angle agrees, within our 6PN accuracy, with the computation of [Phys.\ Rev.\ Lett.\ {\bf 122}, no. 20, 201603 (2019)]. All our results are expressed in several different gauge-invariant ways. We highlight, and make a crucial use of, several aspects of the hidden simplicity of the mass-ratio dependence of the two-body dynamics., Comment: 36 pages, 1 figure

Published
2020
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159. Observing the inspiral of coalescing massive black hole binaries with LISA in the era of multimessenger astrophysics

Author

Stanislav Babak, Alberto Mangiagli, Matteo Bonetti, Marta Volonteri, Sylvain Marsat, Michael L. Katz, Monica Colpi, Alberto Sesana, Antoine Klein, Mangiagli, A, Klein, A, Bonetti, M, Katz, M, Sesana, A, Volonteri, M, Colpi, M, Marsat, S, Babak, S, Institut d'Astrophysique de Paris (IAP), Institut national des sciences de l'Univers (INSU - CNRS)-Sorbonne Université (SU)-Centre National de la Recherche Scientifique (CNRS), AstroParticule et Cosmologie (APC (UMR_7164)), Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Observatoire de Paris, Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Centre National de la Recherche Scientifique (CNRS)-Université Paris Cité (UPCité), and Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Centre National de la Recherche Scientifique (CNRS)-Université de Paris (UP)

Subjects
data analysis method, On the fly, gravitation: model, alternative theories of gravity, FOS: Physical sciences, black hole binaries, LISA, multimessenger, Astrophysics::Cosmology and Extragalactic Astrophysics, Astrophysics, General Relativity and Quantum Cosmology (gr-qc), 01 natural sciences, General Relativity and Quantum Cosmology, localization, Monte Carlo: Markov chain, electromagnetic field: production, FIS/05 - ASTRONOMIA E ASTROFISICA, binary: coalescence, statistical analysis, 0103 physical sciences, black hole, galaxy: redshift: low, Invariant mass, 010306 general physics, Physics, High Energy Astrophysical Phenomena (astro-ph.HE), LISA, 010308 nuclear & particles physics, Computer Science::Information Retrieval, gravitational radiation, Computer Science::Computation and Language (Computational Linguistics and Natural Language and Speech Processing), Laser interferometer space antenna, Mass ratio, Redshift, gravitational radiation detector, detector: sensitivity, General relativity, black hole: binary, gravitational radiation: emission, [PHYS.GRQC]Physics [physics]/General Relativity and Quantum Cosmology [gr-qc], mass ratio, Astrophysics - High Energy Astrophysical Phenomena, [PHYS.ASTR]Physics [physics]/Astrophysics [astro-ph]
Abstract

Massive black hole binaries (MBHBs) of $10^5 \, \rm M_\odot - 3 \times 10^7 \, \rm M_\odot $ merging in low redshift galaxies ($z\le4$) are sufficiently loud to be detected weeks before coalescence with the Laser Interferometer Space Antenna (LISA). This allows us to perform the parameter estimation $on$ $the$ $fly$, i.e. as a function of the time to coalescence during the inspiral phase, relevant for early warning of the planned LISA protected periods and for searches of electromagnetic signals. In this work, we study the evolution of the sky position, luminosity distance, chirp mass and mass ratio uncertainties as function of time left before merger. Overall, light systems with total intrinsic mass $\rm M_{\rm tot} = 3 \times 10^5 \, \rm M_\odot$ are characterized by smaller uncertainties than heavy ones ($\rm M_{\rm tot} = 10^7 \, \rm M_\odot$) during the inspiral. Luminosity distance, chirp mass and mass ratio are well constrained at the end of the inspiral. Concerning sky position, at $z=1$, MBHBs with $\rm M_{\rm tot} = 3 \times 10^5 \, \rm M_\odot$ can be localized with a median precision of $\simeq 10^2 \, \rm deg^2 (\simeq 1 \, \rm deg^2)$ at 1 month (1 hour) from merger, while the sky position of heavy MBHBs can be determined to $10 \, \rm deg^2$ only 1 hour before merger. However the uncertainty around the median values broadens with time, ranging in between 0.04 -- 20 $\rm deg^2$ (0.3 -- 3 $\times 10^3 \, \rm deg^2$) for light (heavy) systems at 1 hour before merger. At merger the sky localization improves down to $\simeq 10^{-1} \, \rm deg^2$ for all masses. For the benefit of the observer community, we provide the full set of data from our simulations and simple and ready-to-use analytical fits to describe the time evolution of uncertainties in the aforementioned parameters, valid for systems with total mass between $10^5$--$10^7 \, \rm M_\odot$ and redshift $0.3$--$3$., Comment: 31 pages, 24 figures and 6 tables. Accepted for publication in Physical Review D

Published
2020
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160. Compact Objects in Entangled Relativity

Author

Olivier Rousselle, Olivier Minazzoli, Denis Arruga, AstroParticule et Cosmologie (APC (UMR_7164)), Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Observatoire de Paris, Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Centre National de la Recherche Scientifique (CNRS)-Université de Paris (UP), Laboratoire Kastler Brossel (LKB [Collège de France]), École normale supérieure - Paris (ENS Paris), Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Centre National de la Recherche Scientifique (CNRS)-Fédération de recherche du Département de physique de l'Ecole Normale Supérieure - ENS Paris (FRDPENS), Centre National de la Recherche Scientifique (CNRS)-École normale supérieure - Paris (ENS Paris), Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Centre National de la Recherche Scientifique (CNRS)-Sorbonne Université (SU)-Collège de France (CdF (institution)), Astrophysique Relativiste Théories Expériences Métrologie Instrumentation Signaux (ARTEMIS), Université Nice Sophia Antipolis (... - 2019) (UNS), COMUE Université Côte d'Azur (2015-2019) (COMUE UCA)-COMUE Université Côte d'Azur (2015-2019) (COMUE UCA)-Institut national des sciences de l'Univers (INSU - CNRS)-Observatoire de la Côte d'Azur, COMUE Université Côte d'Azur (2015-2019) (COMUE UCA)-Université Côte d'Azur (UCA)-Université Côte d'Azur (UCA)-Centre National de la Recherche Scientifique (CNRS), Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Centre National de la Recherche Scientifique (CNRS)-Université Paris Cité (UPCité), Fédération de recherche du Département de physique de l'Ecole Normale Supérieure - ENS Paris (FRDPENS), École normale supérieure - Paris (ENS-PSL), Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Centre National de la Recherche Scientifique (CNRS)-École normale supérieure - Paris (ENS-PSL), Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Centre National de la Recherche Scientifique (CNRS)-Collège de France (CdF (institution))-Sorbonne Université (SU)-Centre National de la Recherche Scientifique (CNRS), and Université Nice Sophia Antipolis (1965 - 2019) (UNS)

Subjects
star: compact, General relativity, alternative theories of gravity, FOS: Physical sciences, Quantum entanglement, General Relativity and Quantum Cosmology (gr-qc), Compact star, 01 natural sciences, General Relativity and Quantum Cosmology, Theoretical physics, Theory of relativity, 0103 physical sciences, conservation law, 010306 general physics, numerical calculations, neutron star, equation of state, Physics, Conservation law, Tolman-Oppenheimer-Volkoff equation, density, 010308 nuclear & particles physics, Equation of state (cosmology), Neutron star, relativity theory, [PHYS.GRQC]Physics [physics]/General Relativity and Quantum Cosmology [gr-qc], entanglement, Free parameter
Abstract

We describe the first numerical Tolman-Oppenheimer-Volkoff solutions of compact objects in entangled relativity, which is an alternative to the framework of general relativity that does not have any additional free parameter. Assuming a simple polytropic equation of state and the conservation of the rest-mass density, we notably show that, for any given density, compact objects are always heavier (up to $\sim 8\%$) in entangled relativity than in general relativity -- for any given central density within the usual range of neutron stars' central densities, or for a given radius of the resulting compact object., Comment: 9 pages, 7 figures

Published
2020
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161. Radiative contribution to classical gravitational scattering at the third order in $G$

Author

Thibault Damour, Institut des Hautes Etudes Scientifiques (IHES), and IHES

Subjects
Physics, 010308 nuclear & particles physics, General relativity, Gravitational wave, Scattering, alternative theories of gravity, Order (ring theory), FOS: Physical sciences, General Relativity and Quantum Cosmology (gr-qc), 01 natural sciences, General Relativity and Quantum Cosmology, Gravitation, Massless particle, 0103 physical sciences, [PHYS.GRQC]Physics [physics]/General Relativity and Quantum Cosmology [gr-qc], Radiative transfer, 010306 general physics, Mathematical physics, Sign (mathematics)
Abstract

Working within the post-Minkowskian approach to General Relativity, we prove that the radiation-reaction to the emission of gravitational waves during the large-impact-parameter scattering of two (classical) point masses modifies the conservative scattering angle by an additional contribution of order $G^3$ which involves a high-energy (or massless) logarithmic divergence of opposite sign to the one contained in the third-post-Minkowskian result of Bern et al. [Phys. Rev. Lett. {\bf 122}, 201603 (2019)]. The high-energy limit of the resulting radiation-reaction-corrected (classical) scattering angle is finite, and is found to agree with the one following from the (quantum) eikonal-phase result of Amati, Ciafaloni and Veneziano [ Nucl. Phys. B {\bf 347}, 550 (1990)]., Comment: 10 pages, no figures

Published
2020
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162. Constraining velocity-dependent Lorentz/CPT-violations using Lunar Laser Ranging

Author

G. Francou, J. J. Howard, M. C. Angonin, Adrien Bourgoin, Quentin G. Bailey, Clément Courde, Julien Chabé, J.-M. Torre, Aurélien Hees, S. Bouquillon, C. Le Poncin-Lafitte, Systèmes de Référence Temps Espace (SYRTE), Institut national des sciences de l'Univers (INSU - CNRS)-Observatoire de Paris, Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Sorbonne Université (SU)-Centre National de la Recherche Scientifique (CNRS), Géoazur (GEOAZUR 7329), Institut national des sciences de l'Univers (INSU - CNRS)-Observatoire de la Côte d'Azur, and COMUE Université Côte d'Azur (2015-2019) (COMUE UCA)-Université Côte d'Azur (UCA)-COMUE Université Côte d'Azur (2015-2019) (COMUE UCA)-Université Côte d'Azur (UCA)-Centre National de la Recherche Scientifique (CNRS)-Institut de Recherche pour le Développement (IRD [France-Sud])

Subjects
velocity, Physics::General Physics, constraint, Lorentz transformation, alternative theories of gravity, FOS: Physical sciences, CPT: violation, General Relativity and Quantum Cosmology (gr-qc), 01 natural sciences, General Relativity and Quantum Cosmology, Gravitation, symbols.namesake, Theoretical physics, Standard-Model Extension, 0103 physical sciences, operator: dimension: 5, lunar, 010306 general physics, pulsar, Physics, [PHYS]Physics [physics], 010308 nuclear & particles physics, High Energy Physics::Phenomenology, Relative velocity, Equations of motion, field equations, violation: Lorentz, laser, Orders of magnitude (time), General relativity, gravitation, Homogeneous space, [PHYS.GRQC]Physics [physics]/General Relativity and Quantum Cosmology [gr-qc], symbols, velocity dependence, [PHYS.ASTR]Physics [physics]/Astrophysics [astro-ph], Jackknife resampling
Abstract

The possibility for Lorentz/CPT-breaking, which is motivated by unification theories, can be systematically tested within the standard-model extension framework. In the pure gravity sector, the mass dimension 5 operators produce new Lorentz and CPT-breaking terms in the 2-body equations of motion that depend on the relative velocity of the bodies. In this Letter, we report new constraints on 15 independent SME coefficients for Lorentz/CPT-violations with mass dimension 5 using lunar laser ranging. We perform a global analysis of lunar ranging data within the SME framework using more than 26,000 normal points between 1969 and 2018. We also perform a jackknife analysis in order to provide realistic estimates of the systematic uncertainties. No deviation from Lorentz/CPT symmetries is reported. In addition, when fitting simultaneously for the 15 canonical SME coefficients for Lorentz/CPT-violations, we improve up to three orders of magnitude previous post-fit constraints from radio pulsars., Comment: 8 pages, 1 figure

Published
2020
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163. Motion of localized sources in general relativity: Gravitational self-force from quasilocal conservation laws

Author

Richard J. Epp, Robert B. Mann, Marius Oltean, Carlos F. Sopuerta, Alessandro D. A. M. Spallicci, Natural Sciences and Engineering Research Council of Canada, Ministerio de Economía y Competitividad (España), Ministerio de Ciencia, Innovación y Universidades (España), Agencia Estatal de Investigación (España), Generalitat de Catalunya, European Commission, Laboratoire de Physique et Chimie de l'Environnement et de l'Espace (LPC2E), Observatoire des Sciences de l'Univers en région Centre (OSUC), Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS)-Université d'Orléans (UO)-Observatoire de Paris, PSL Research University (PSL)-PSL Research University (PSL)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS)-Université d'Orléans (UO)-Observatoire de Paris, PSL Research University (PSL)-PSL Research University (PSL)-Centre National d’Études Spatiales [Paris] (CNES), Université d'Orléans (UO), Institut national des sciences de l'Univers (INSU - CNRS)-Observatoire de Paris, Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Université d'Orléans (UO)-Centre National de la Recherche Scientifique (CNRS)-Institut national des sciences de l'Univers (INSU - CNRS)-Observatoire de Paris, and Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Université d'Orléans (UO)-Centre National de la Recherche Scientifique (CNRS)-Centre National d’Études Spatiales [Paris] (CNES)

Subjects
High Energy Physics - Theory, Geodesic, General relativity, gravitation: effect, alternative theories of gravity, FOS: Physical sciences, General Relativity and Quantum Cosmology (gr-qc), gravitational radiation: direct detection, 01 natural sciences, General Relativity and Quantum Cosmology, Motion (physics), Gravitation, 0103 physical sciences, general relativity, conservation law, numerical calculations, 010306 general physics, Physics, High Energy Astrophysical Phenomena (astro-ph.HE), LISA, Conservation law, Spacetime, [PHYS.HTHE]Physics [physics]/High Energy Physics - Theory [hep-th], 010308 nuclear & particles physics, Gravitational wave, Equations of motion, field equations, metric: Kerr, momentum: flux, gravitational radiation detector, Classical mechanics, High Energy Physics - Theory (hep-th), [SDU]Sciences of the Universe [physics], curvature, gravitational radiation: emission, gravitation: self-force, [PHYS.GRQC]Physics [physics]/General Relativity and Quantum Cosmology [gr-qc], Astrophysics - High Energy Astrophysical Phenomena, mass: finite, [PHYS.ASTR]Physics [physics]/Astrophysics [astro-ph], geodesic
Abstract

An idealized “test” object in general relativity moves along a geodesic. However, if the object has a finite mass, this will create additional curvature in the spacetime, causing it to deviate from geodesic motion. If the mass is nonetheless sufficiently small, such an effect is usually treated perturbatively and is known as the gravitational self-force due to the object. This issue is still an open problem in gravitational physics today, motivated not only by basic foundational interest, but also by the need for its direct application in gravitational wave astronomy. In particular, the observation of extreme-mass-ratio inspirals by the future space-based detector LISA will rely crucially on an accurate modeling of the self-force driving the orbital evolution and gravitational wave emission of such systems. In this paper, we present a novel derivation, based on conservation laws, of the basic equations of motion for this problem. They are formulated with the use of a quasilocal (rather than matter) stress-energy-momentum tensor—in particular, the Brown-York tensor—so as to capture gravitational effects in the momentum flux of the object, including the self-force. Our formulation and resulting equations of motion are independent of the choice of the perturbative gauge. We show that, in addition to the usual gravitational self-force term, they also lead to an additional “self-pressure” force not found in previous analyses, and also that our results correctly recover known formulas under appropriate conditions. Our approach thus offers a fresh geometrical picture from which to understand the self-force fundamentally, and potentially useful new avenues for computing it practically., M. O. and R. B. M. acknowledge support from the Natural Sciences and Engineering Research Council of Canada. M. O. and C. F. S. acknowledge support from Contracts No. ESP2013-47637-P, No. ESP2015-67234-P, and No. ESP2017-90084-P from the Ministry of Economy and Business of Spain (MINECO) and from Contract No. 2017-SGR-1469 from AGAUR (Catalan government). M. O. and A. D. A. M. S. acknowledge LISA CNES funding. We also acknowledge networking support by the COST Action GWverse CA16104 (Horizon 2020 Framework Programme of the European Union).

Published
2020
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164. Late-time cosmological evolution in degenerate higher-order scalar-tensor models

Author

Hamza Boumaza, Karim Noui, David Langlois, AstroParticule et Cosmologie (APC (UMR_7164)), Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Observatoire de Paris, Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Centre National de la Recherche Scientifique (CNRS)-Université de Paris (UP), and Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Centre National de la Recherche Scientifique (CNRS)-Université Paris Cité (UPCité)

Subjects
velocity, cosmological model, General relativity, perturbation, gravitation: model, Perturbation (astronomy), alternative theories of gravity, Parameter space, 01 natural sciences, photon: velocity, Theoretical physics, General Relativity and Quantum Cosmology, Quadratic equation, 0103 physical sciences, Friedman model, 010306 general physics, dark energy, Physics, matter: nonrelativistic, 010308 nuclear & particles physics, Gravitational wave, [PHYS.HTHE]Physics [physics]/High Energy Physics - Theory [hep-th], Degenerate energy levels, gravitational radiation, stability, field theory: scalar, Wavelength, gravitation: scalar tensor, evolution equation, Dark energy, [PHYS.GRQC]Physics [physics]/General Relativity and Quantum Cosmology [gr-qc], gravitation: higher-order, [PHYS.ASTR]Physics [physics]/Astrophysics [astro-ph], dark energy: equation of state
Abstract

International audience; We study the late cosmological evolution, from the nonrelativistic matter dominated era to the dark energy era, in modified gravity models described by degenerate higher-order scalar-tensor (DHOST) theories. They represent the most general scalar-tensor theories propagating a single scalar degree of freedom and include Horndeski and beyond Horndeski theories. We provide the homogeneous evolution equations for any quadratic DHOST theory, without restricting ourselves to theories where the speed of gravitational waves coincides with that of light since the present constraints apply to wavelengths much smaller than cosmological scales. To illustrate the potential richness of the cosmological background evolution in these theories, we consider a simple family of shift-symmetric models, characterized by three parameters and compute the evolution of dark energy and of its equation of state. We also identify the regions in parameter space where the models are perturbatively stable.

Published
2020
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165. 1+3 formulation of Newton’s equations

Author

Quentin Vigneron, Centre de Recherche Astrophysique de Lyon (CRAL), École normale supérieure - Lyon (ENS Lyon)-Université Claude Bernard Lyon 1 (UCBL), Université de Lyon-Université de Lyon-Centre National de la Recherche Scientifique (CNRS)-Institut national des sciences de l'Univers (INSU - CNRS), École normale supérieure de Lyon (ENS de Lyon)-Université Claude Bernard Lyon 1 (UCBL), and Université de Lyon-Université de Lyon-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS)

Subjects
Physics, Cosmology and Nongalactic Astrophysics (astro-ph.CO), Spacetime, 010308 nuclear & particles physics, General relativity, Coordinate system, FOS: Physical sciences, alternative theories of gravity, General Relativity and Quantum Cosmology (gr-qc), Newtonian limit, Conservative vector field, 01 natural sciences, General Relativity and Quantum Cosmology, Gravitation, 0103 physical sciences, Newtonian fluid, [PHYS.GRQC]Physics [physics]/General Relativity and Quantum Cosmology [gr-qc], 010306 general physics, [PHYS.ASTR]Physics [physics]/Astrophysics [astro-ph], Schwarzschild radius, Mathematical physics, Astrophysics - Cosmology and Nongalactic Astrophysics
Abstract

We present in this paper a 4-dimensional formulation of the Newton equations for gravitation on a Lorentzian manifold, inspired from the 1+3 and 3+1 formalisms of general relativity. We first show that the freedom on the coordinate velocity of a general time-parametrised coordinate system with respect to a Galilean reference system is similar to the shift freedom in the 3+1-formalism of general relativity. This allows us to write Newton's theory as living in a 4-dimensional Lorentzian manifold $M^N$. This manifold can be chosen to be curved depending on the dynamics of the Newtonian fluid. In this paper, we focus on a specific choice for $M^N$ leading to what we call the \textit{1+3-Newton equations}. We show that these equations can be recovered from general relativity with a Newtonian limit performed in the rest frames of the relativistic fluid. The 1+3 formulation of the Newton equations along with the Newtonian limit we introduce also allow us to define a dictionary between Newton's theory and general relativity. This dictionary is defined in the rest frames of the dust fluid, i.e. a non-accelerating observer. A consequence of this is that it is only defined for irrotational fluids. As an example supporting the 1+3-Newton equations and our dictionary, we show that the parabolic free-fall solution in 1+3-Newton exactly translates into the Schwarzschild spacetime, and this without any approximations. The dictionary might then be an additional tool to test the validity of Newtonian solutions with respect to general relativity. It however needs to be further tested for non-vacuum, non-stationary and non-isolated Newtonian solutions, as well as to be adapted for rotational fluids. One of the main applications we consider for the 1+3 formulation of Newton's equations is to define new models suited for the study of backreaction and global topology in cosmology., Accepted for publication in Physical Review D; 26 pages, 2 figures

Published
2020
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166. Fifth force induced by a chameleon field on nested cylinders

Author

Jean-Philippe Uzan, Philippe Brax, Martin Pernot-Borràs, Joel Bergé, ONERA - The French Aerospace Lab [Châtillon], ONERA-Université Paris Saclay (COmUE), Institut d'Astrophysique de Paris (IAP), Institut national des sciences de l'Univers (INSU - CNRS)-Sorbonne Université (SU)-Centre National de la Recherche Scientifique (CNRS), Institut de Physique Théorique - UMR CNRS 3681 (IPHT), Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Université Paris-Saclay-Centre National de la Recherche Scientifique (CNRS), Institut Lagrange de Paris, and Sorbonne Université (SU)

Subjects
chameleon, cosmological model, Cosmology and Nongalactic Astrophysics (astro-ph.CO), geometry, Field (physics), symmetry: cylinder, FOS: Physical sciences, alternative theories of gravity, Context (language use), General Relativity and Quantum Cosmology (gr-qc), 01 natural sciences, General Relativity and Quantum Cosmology, Gravitation, 0103 physical sciences, numerical methods, propagation, medicine, 010306 general physics, dimension: 2, numerical calculations, Scaling, Physics, 010308 nuclear & particles physics, screening, Fifth force, Scalar (physics), Stiffness, Symmetry (physics), field theory: scalar, fifth force, Classical mechanics, gravitation: scalar tensor, General relativity, gravitation, [PHYS.GRQC]Physics [physics]/General Relativity and Quantum Cosmology [gr-qc], medicine.symptom, [PHYS.ASTR]Physics [physics]/Astrophysics [astro-ph], Astrophysics - Cosmology and Nongalactic Astrophysics
Abstract

This article investigates the properties of a scalar fifth force that arises in a scalar tensor-theory with a chameleon screening mechanism in the context of gravity space missions like the MICROSCOPE experiment. In such an experiment, the propagation of the chameleon field inside the nested cylinders of the experiment causes a fifth force when the cylinders are not perfectly co-axial. We propose a semi-analytic method to compute the field distribution and the induced fifth force and compare it to a full numerical simulation, in settings where the cylindrical symmetry is broken. The scaling of the fifth force with both the parameters of the model and the geometry of the experiment is discussed. We show that the fifth force is repulsive, hence adds a destabilizing stiffness that should be included in the force budget acting on the detector. This opens the way to a new method to constrain a scalar fifth force in screened models., Comment: Submitted to Phys. Rev. D

Published
2020
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167. Identifying and Addressing Nonstationary LISA Noise

Author

Patricio Maturana-Russel, Natalia Korsakova, Nelson Christensen, Jonathan R. Gair, M. C. Edwards, Renate Meyer, Astrophysique Relativiste Théories Expériences Métrologie Instrumentation Signaux (ARTEMIS), Université Nice Sophia Antipolis (... - 2019) (UNS), COMUE Université Côte d'Azur (2015-2019) (COMUE UCA)-COMUE Université Côte d'Azur (2015-2019) (COMUE UCA)-Institut national des sciences de l'Univers (INSU - CNRS)-Observatoire de la Côte d'Azur, and COMUE Université Côte d'Azur (2015-2019) (COMUE UCA)-Université Côte d'Azur (UCA)-Université Côte d'Azur (UCA)-Centre National de la Recherche Scientifique (CNRS)

Subjects
Noise power, noise, data analysis method, detector: satellite, FOS: Physical sciences, alternative theories of gravity, detector: noise, General Relativity and Quantum Cosmology (gr-qc), 01 natural sciences, General Relativity and Quantum Cosmology, Surrogate data, statistical analysis, 0103 physical sciences, Electronic engineering, [PHYS.PHYS.PHYS-INS-DET]Physics [physics]/Physics [physics]/Instrumentation and Detectors [physics.ins-det], 010306 general physics, numerical calculations, Instrumentation and Methods for Astrophysics (astro-ph.IM), Statistical hypothesis testing, Physics, LISA, density: spectral, white dwarf: binary, 010308 nuclear & particles physics, Gravitational wave, Estimation theory, gravitational radiation, Astrophysics::Instrumentation and Methods for Astrophysics, Spectral density, gravitational radiation detector, Noise, Pathfinder, General relativity, gravitational radiation: emission, Physics::Space Physics, [PHYS.GRQC]Physics [physics]/General Relativity and Quantum Cosmology [gr-qc], galaxy, Astrophysics - Instrumentation and Methods for Astrophysics
Abstract

We anticipate noise from the Laser Interferometer Space Antenna (LISA) will exhibit nonstationarities throughout the duration of its mission due to factors such as antenna repointing, cyclostationarities from spacecraft motion, and glitches as highlighted by LISA Pathfinder. In this paper, we use a surrogate data approach to test the stationarity of a time series which does not rely on the Gaussianity assumption. The main goal is to identify noise nonstationarities in the future LISA mission. This will be necessary for determining how often the LISA noise power spectral density (PSD) will need to be updated for parameter estimation routines. We conduct a thorough simulation study illustrating the power/size of various versions of the hypothesis tests, and then apply these approaches to differential acceleration measurements from LISA Pathfinder. We also develop a data analysis strategy for addressing nonstationarities in the LISA PSD, where we update the noise PSD over time, while simultaneously conducting parameter estimation, with a focus on planned data gaps., Comment: 19 pages, 17 figures

Published
2020
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168. Tidal effects in the equations of motion of compact binary systems to next-to-next-to-leading post-Newtonian order

Author

Luc Blanchet, Guillaume Faye, Quentin Henry, Institut d'Astrophysique de Paris (IAP), and Institut national des sciences de l'Univers (INSU - CNRS)-Sorbonne Université (SU)-Centre National de la Recherche Scientifique (CNRS)

Subjects
Harmonic coordinates, Physics, 010308 nuclear & particles physics, Computation, FOS: Physical sciences, Binary number, Equations of motion, alternative theories of gravity, General Relativity and Quantum Cosmology (gr-qc), 01 natural sciences, General Relativity and Quantum Cosmology, symbols.namesake, Classical mechanics, General relativity, Polarizability, 0103 physical sciences, Tidal force, Newtonian fluid, symbols, [PHYS.GRQC]Physics [physics]/General Relativity and Quantum Cosmology [gr-qc], 010306 general physics, Hamiltonian (quantum mechanics)
Abstract

As a first step in the computation of the orbital phase evolution of spinless compact binaries including tidal effects up to the next-to-next-to-leading (NNL) order, we obtain the equations of motion of those systems and the associated conserved integrals in harmonic coordinates. The internal structure and finite size effects of the compact objects are described by means of an effective Fokker-type action. Our results, complete to the NNL order, correspond to the second-post-Newtonian (2PN) approximation beyond the leading tidal effect itself, already occurring at the 5PN order. They are parametrized by three polarizability (or deformability) coefficients describing the mass quadrupolar, mass octupolar and current quadrupolar deformations of the objects through tidal interactions. Up to the next-to-leading (NL) order, we recover previous results in the literature; up to the NNL order for quasi-circular orbits, we confirm the known tidal effects in the (PN re-expansion of the) effective-one-body (EOB) Hamiltonian. In a future work, we shall derive the tidal contributions to the gravitational-wave flux up to the NNL order, which is the second step required to find the orbital phase evolution., 21 pages

Published
2020
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169. Probing modified gravity theories and cosmology using gravitational-waves and associated electromagnetic counterparts

Author

S. Mastrogiovanni, Daniele A. Steer, M. Barsuglia, AstroParticule et Cosmologie (APC (UMR_7164)), Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Observatoire de Paris, Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Centre National de la Recherche Scientifique (CNRS)-Université de Paris (UP), Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Centre National de la Recherche Scientifique (CNRS)-Université Paris Cité (UPCité), and ANR-18-IDEX-0001,Université de Paris,Université de Paris(2018)

Subjects
cosmological model, neutron star: binary, General relativity, dispersion relation, gravitation: model, Astrophysics::High Energy Astrophysical Phenomena, FOS: Physical sciences, alternative theories of gravity, General Relativity and Quantum Cosmology (gr-qc), Astrophysics, Astrophysics::Cosmology and Extragalactic Astrophysics, gamma ray: burst, gravitational radiation: direct detection, 01 natural sciences, space-time: Robertson-Walker, General Relativity and Quantum Cosmology, Cosmology, Monte Carlo: Markov chain, electromagnetic field: production, symbols.namesake, phase shift, gravitational radiation: propagation, gravitation: weak field, 0103 physical sciences, general relativity, LIGO, 010306 general physics, gravitational radiation: frequency, Physics, [PHYS]Physics [physics], Hubble constant, 010308 nuclear & particles physics, Gravitational wave, gravitational radiation, Order (ring theory), statistical analysis: Bayesian, time delay, Neutron star, Massive gravity, VIRGO, gravitational radiation: emission, symbols, [PHYS.GRQC]Physics [physics]/General Relativity and Quantum Cosmology [gr-qc], galaxy, [PHYS.ASTR]Physics [physics]/Astrophysics [astro-ph], geodesic, Hubble's law
Abstract

The direct detection of gravitational waves by the LIGO-Virgo collaboration has opened a new window with which to measure cosmological parameters such as the Hubble constant $H_0$, and also probe general relativity on large scales. In this paper we present a new phenomenological approach, together with its inferencial implementation, for measuring deviations from general relativity (GR) on cosmological scales concurrently with a determination of $H_0$. We consider gravitational waves (GWs) propagating in an expanding homogeneous and isotropic background, but with a modified friction term and dispersion relation relative to that of GR. We find that a single binary neutron star GW detection will poorly constrain the GW friction term. However, a joint analysis including the GW phase and GW-GRB detection delay could improve constraints on some GW dispersion relations provided the delay is measured with millisecond precision. We also show that, for massive gravity, by combining 100 binary neutron stars detections with observed electromagnetic counterparts and hosting galaxy identification, we will be able to constrain the Hubble constant, the GW damping term and the GW dispersion relation with 2\%, 15\% and 2 \% accuracy, respectively. We emphasise that these three parameters should be measured together in order avoid biases. Finally we apply the method to GW170817, and demonstrate that for all the GW dispersions relations we consider, including massive gravity, the GW must be emitted $\sim$ 1.74s before the Gamma-ray burst (GRB). Furthermore, at the GW merger peak frequency, we show that the fractional difference between the GW group velocity and $c$ is $\lesssim 10^{-17}$., Comment: 19 pages, 13 Figs

Published
2020
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170. Tidal effects in the gravitational-wave phase evolution of compact binary systems to next-to-next-to-leading post-Newtonian order

Author

Guillaume Faye, Quentin Henry, Luc Blanchet, Institut d'Astrophysique de Paris (IAP), and Institut national des sciences de l'Univers (INSU - CNRS)-Sorbonne Université (SU)-Centre National de la Recherche Scientifique (CNRS)

Subjects
Physics, 010308 nuclear & particles physics, Gravitational wave, FOS: Physical sciences, Energy flux, Equations of motion, Binary number, alternative theories of gravity, General Relativity and Quantum Cosmology (gr-qc), 01 natural sciences, Phase evolution, General Relativity and Quantum Cosmology, General relativity, Quantum electrodynamics, 0103 physical sciences, Newtonian fluid, [PHYS.GRQC]Physics [physics]/General Relativity and Quantum Cosmology [gr-qc], Binary system, 010306 general physics, Multipole expansion
Abstract

We compute the gravitational-wave (GW) energy flux up to the next-to-next-to-leading (NNL) order of tidal effects in a spinless compact binary system on quasi-circular orbits. Starting from an effective matter action, we obtain the stress-energy tensor of the system, which we use in a GW generation formalism based on multipolar-post-Minkowskian (MPM) and post-Newtonian (PN) approximations. The tidal contributions to the multipole moments of the system are first obtained, from which we deduce the instantaneous GW energy flux to NNL order (formally 7PN order). We also include the remaining tidal contributions of GW tails to the leading (formally 6.5PN) and NL (7.5PN) orders. Combining it with our previous work on the conservative equations of motion (EoM) and associated energy, we get the GW phase and frequency evolution through the flux-balance equation to the same NNL order. These results extend and complete several preceding results in the literature., 26 pages

Published
2020
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171. TEST PARTICLES BEHAVIOR IN THE FRAMEWORK OF A LAGRANGIAN GEOMETRIC THEORY WITH PROPAGATING TORSION.

Author

Aprea, G., Montani, G., and Ruffini, R.

Subjects
*TORSION, *GRAVITATIONAL fields, *GEOMETRIC measure theory, *LAGRANGE equations, *STRAINS & stresses (Mechanics), *GRAVITY waves
Abstract

Working in the Lagrangian framework, we develop a geometric theory in vacuum with propagating torsion; the antisymmetric and trace parts of the torsion tensor, considered as derived from local potential fields, are taken and, using the minimal action principle, their field equations are calculated. Actually these will show themselves to be just equations for propagating waves giving torsion a behavior similar to that of metric which, as known, propagates through gravitational waves. Then we establish a principle of minimal substitution to derive test particles equation of motion, obtaining, as result, that they move along autoparallels. We then calculate the analogous of the geodesic deviation for these trajectories and analyze their behavior in the nonrelativistic limit, showing that the torsion trace potential ϕ has a phenomenology which is indistinguishable from that of the gravitational newtonian field; in this way we also give a reason for why there have never been evidence for it. [ABSTRACT FROM AUTHOR]

Published
2003
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172. The Classical Symmetron Force in Casimir Experiments

Author

Anne-Christine Davis, Philippe Brax, Benjamin Elder, Valeri Vardanyan, Yashar Akrami, Ricardo S. Decca, Laboratoire de physique de l'ENS - ENS Paris (LPENS (UMR_8023)), École normale supérieure - Paris (ENS Paris), Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Centre National de la Recherche Scientifique (CNRS)-Sorbonne Université (SU)-Université Paris Diderot - Paris 7 (UPD7), Laboratoire d'Etude du Rayonnement et de la Matière en Astrophysique (LERMA (UMR_8112)), Sorbonne Université (SU)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS)-Université de Cergy Pontoise (UCP), Université Paris-Seine-Université Paris-Seine-Observatoire de Paris, Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL), Institut de Physique Théorique - UMR CNRS 3681 (IPHT), Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Université Paris-Saclay-Centre National de la Recherche Scientifique (CNRS), École normale supérieure - Paris (ENS-PSL), Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Université Paris Diderot - Paris 7 (UPD7)-Sorbonne Université (SU)-Centre National de la Recherche Scientifique (CNRS), Institut national des sciences de l'Univers (INSU - CNRS)-Observatoire de Paris, Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Université de Cergy Pontoise (UCP), Université Paris-Seine-Université Paris-Seine-Sorbonne Université (SU)-Centre National de la Recherche Scientifique (CNRS), Fédération de recherche du Département de physique de l'Ecole Normale Supérieure - ENS Paris (FRDPENS), Centre National de la Recherche Scientifique (CNRS)-École normale supérieure - Paris (ENS Paris)-Centre National de la Recherche Scientifique (CNRS)-École normale supérieure - Paris (ENS Paris)-Université Paris Diderot - Paris 7 (UPD7)-Sorbonne Université (SU)-Centre National de la Recherche Scientifique (CNRS), and PSL Research University (PSL)-PSL Research University (PSL)-Université de Cergy Pontoise (UCP)

Subjects
Atom interferometer, Gravity (chemistry), Cosmology and Nongalactic Astrophysics (astro-ph.CO), experimental methods, General relativity, gravitation: model, FOS: Physical sciences, alternative theories of gravity, General Relativity and Quantum Cosmology (gr-qc), Space (mathematics), 01 natural sciences, General Relativity and Quantum Cosmology, High Energy Physics - Phenomenology (hep-ph), invariance: scale, 0103 physical sciences, numerical methods, field theory: screening, 010306 general physics, numerical calculations, Physics, force: Casimir, 010308 nuclear & particles physics, Numerical analysis, Equations of motion, field equations, atom: interferometer, field theory: scalar, Casimir effect, High Energy Physics - Phenomenology, Classical mechanics, experimental equipment, [PHYS.HPHE]Physics [physics]/High Energy Physics - Phenomenology [hep-ph], [PHYS.GRQC]Physics [physics]/General Relativity and Quantum Cosmology [gr-qc], SPHERES, [PHYS.ASTR]Physics [physics]/Astrophysics [astro-ph], symmetron, Astrophysics - Cosmology and Nongalactic Astrophysics
Abstract

The symmetron is a typical example of screened modified gravity, wherein the symmetron force is dynamically suppressed in dense environments. This allows it to hide in traditional tests of gravity. However, the past decade has seen great experimental progress towards measuring screened forces in the laboratory or in space. Screening relies on nonlinearities in the equation of motion, which significantly complicates the theoretical analysis of such forces. Here, we present a calculation of the symmetron force between a dense plate and sphere surrounded by vacuum. This is done via semi-analytical approaches in two limiting cases, based on the size of the sphere: large spheres are analyzed via the proximity force approximation, whilst small spheres are treated as screened test particles. In the intermediate regime we solve the problem numerically. Our results allow us to make contact with Casimir force experiments, which often employ a plate and sphere configuration for practical reasons, and may therefore be used to constrain symmetrons. We use our results to forecast constraints on the symmetron's parameters for a hypothetical Casimir experiment that is based on the current state of the art. The forecasts compare favorably to other leading laboratory tests of gravity, particularly atom interferometry and bouncing neutrons. We thus conclude that near-future Casimir experiments will be capable of placing tight new bounds on symmetrons. Our results for the symmetron force are derived in a scale-invariant way, such that although we here focus on Casimir experiments, they may be applied to any other plate-sphere system, ranging from microscopic to astrophysical scales., 16 pages, 8 figures

Published
2019
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173. Excited hairy black holes: dynamical construction and level transitions

Author

Hugo Roussille, Pablo Bosch, Stephen R. Green, Luis Lehner, AstroParticule et Cosmologie (APC (UMR_7164)), Observatoire de Paris, PSL Research University (PSL)-PSL Research University (PSL)-Université Paris Diderot - Paris 7 (UPD7)-Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Centre National de la Recherche Scientifique (CNRS), Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Observatoire de Paris, Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Centre National de la Recherche Scientifique (CNRS)-Université de Paris (UP), Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Centre National de la Recherche Scientifique (CNRS)-Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Observatoire de Paris, PSL Research University (PSL)-PSL Research University (PSL)-Université Paris Diderot - Paris 7 (UPD7), and Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Centre National de la Recherche Scientifique (CNRS)-Université Paris Cité (UPCité)

Subjects
High Energy Physics - Theory, family, black hole: Reissner-Nordstroem, field theory: scalar: massive, 01 natural sciences, General Relativity and Quantum Cosmology, Reissner-Nordstroem, symmetry: rotation, black hole: hair, [PHYS]Physics [physics], Physics, [PHYS.HTHE]Physics [physics]/High Energy Physics - Theory [hep-th], condensation: scalar, perturbation: scalar, General relativity, Excited state, Quantum electrodynamics, [PHYS.GRQC]Physics [physics]/General Relativity and Quantum Cosmology [gr-qc], Circular symmetry, Scalar field, background: anti-de Sitter, Field (physics), Thermodynamic equilibrium, perturbation, coupling: gauge, Scalar (mathematics), FOS: Physical sciences, alternative theories of gravity, General Relativity and Quantum Cosmology (gr-qc), Instability, horizon, 0103 physical sciences, 010306 general physics, numerical calculations, charge: electric, 010308 nuclear & particles physics, quasinormal mode, stability, black hole: anti-de Sitter, tracks, boundary condition, field theory: scalar, Black hole, Automatic Keywords, High Energy Physics - Theory (hep-th), nonlinear, approximation: linear, [PHYS.ASTR]Physics [physics]/Astrophysics [astro-ph], superradiance
Abstract

We study the dynamics of unstable Reissner-Nordstr\"om anti-de Sitter black holes under charged scalar field perturbations in spherical symmetry. We unravel their general behavior and approach to the final equlibrium state. In the first part of this work, we present a numerical analysis of massive charged scalar field quasinormal modes. We identify the known mode families - superradiant modes, zero-damped modes, AdS modes, and the near-horizon mode - and we track their migration under variation of the black hole and field parameters. We show that the zero-damped modes become superradiantly unstable for large RNAdS with large gauge coupling; the leading unstable mode is identified with the near-horizon condensation instability. In the second part, we present results of numerical simulations of perturbed large RNAdS, showing the nonlinear development of these unstable modes. For generic initial conditions, charge and mass are ransferred from the black hole to the scalar field, until an equilibrium solution with a scalar condensate is reached. We use results from the linear analysis, however, to select special initial data corresponding to an unstable overtone mode. We find that these data evolve to produce a new equilibrium state - an excited hairy black hole with the scalar condensate in an overtone configuration. This state is, however, unstable, and the black hole eventually decays to the generic end state. Nevertheless, this demonstrates the potential relevance of overtone modes as transients in black hole dynamics., Comment: 16 pages, 17 figures

Published
2019
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174. Self-force effects on the marginally bound zoom-whirl orbit in Schwarzschild spacetime

Author

Soichiro Isoyama, Marta Colleoni, Norichika Sago, Thibault Damour, Leor Barack, Institut des Hautes Etudes Scientifiques (IHES), and IHES

Subjects
High Energy Astrophysical Phenomena (astro-ph.HE), Physics, Angular momentum, Geodesic, 010308 nuclear & particles physics, FOS: Physical sciences, alternative theories of gravity, Perturbation (astronomy), General Relativity and Quantum Cosmology (gr-qc), 01 natural sciences, General Relativity and Quantum Cosmology, Gravitation, Classical mechanics, General relativity, 0103 physical sciences, [PHYS.GRQC]Physics [physics]/General Relativity and Quantum Cosmology [gr-qc], Radiative transfer, Circular orbit, Test particle, Astrophysics - High Energy Astrophysical Phenomena, [PHYS.ASTR]Physics [physics]/Astrophysics [astro-ph], 010306 general physics, Schwarzschild radius
Abstract

For a Schwarzchild black hole of mass $M$, we consider a test particle falling from rest at infinity and becoming trapped, at late time, on the unstable circular orbit of radius $r=4GM/c^2$. When the particle is endowed with a small mass, $\mu\ll M$, it experiences an effective gravitational self-force, whose conservative piece shifts the critical value of the angular momentum and the frequency of the asymptotic circular orbit away from their geodesic values. By directly integrating the self-force along the orbit (ignoring radiative dissipation), we numerically calculate these shifts to $O(\mu/M)$. Our numerical values are found to be in agreement with estimates first made within the Effective One Body formalism, and with predictions of the first law of black-hole-binary mechanics (as applied to the asymptotic circular orbit). Our calculation is based on a time-domain integration of the Lorenz-gauge perturbation equations, and it is a first such calculation for an unbound orbit. We tackle several technical difficulties specific to unbound orbits, illustrating how these may be handled in more general cases of unbound motion. Our method paves the way to calculations of the self-force along hyperbolic-type scattering orbits. Such orbits can probe the two-body potential down to the "light ring", and could thus supply strong-field calibration data for eccentricity-dependent terms in the Effective One Body model of merging binaries., Comment: 29 pages, 6 figures

Published
2019
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175. Classical and quantum scattering in post-Minkowskian gravity

Author

Thibault Damour, Institut des Hautes Etudes Scientifiques (IHES), and IHES

Subjects
scattering: classical, Computation, alternative theories of gravity, FOS: Physical sciences, General Relativity and Quantum Cosmology (gr-qc), 01 natural sciences, General Relativity and Quantum Cosmology, symbols.namesake, 0103 physical sciences, high energy behavior, quantization: 3, 010306 general physics, Mathematical physics, Physics, 010308 nuclear & particles physics, Scattering, scattering amplitude, mass dependence, Hamiltonian, Scattering amplitude, Automatic Keywords, Amplitude, General relativity, gravitation, [PHYS.GRQC]Physics [physics]/General Relativity and Quantum Cosmology [gr-qc], symbols, Scattering theory, self-force, Hamiltonian (quantum mechanics)
Abstract

New structural properties of post-Minkowskian (PM) gravity are derived, notably within its effective one body (EOB) formulation. Our results concern both the mass dependence, and the high-energy behavior, of the classical scattering angle. We generalize our previous work by deriving, up to the fourth post-Minkowskian (4PM) level included, the explicit links between the scattering angle and the two types of potentials entering the Hamiltonian description of PM dynamics within EOB theory. We compute the scattering amplitude derived from quantizing the third post-Minkowskian (3PM) EOB radial potential (including the contributions coming from the Born iterations), and point out various subtleties in the relation between perturbative amplitudes and classical dynamics. We highlight an apparent tension between the classical 3PM dynamics derived by Bern et al. [Phys. Rev. Lett. 122, 201603 (2019)], and previous high-energy self-force results [Phys. Rev. D 86, 104041 (2012)], and propose several possible resolutions of this tension. We point out that linear-in-mass-ratio self-force computations can give access to the exact 3PM and 4PM dynamics., 39 pages, no figures; agrees with published version

Published
2019
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176. Comparing Effective One Body Hamiltonians for spin-aligned coalescing binaries

Author

Fabio Martinetti, Thibault Damour, Gunnar Riemenschneider, Alessandro Nagar, Piero Rettegno, Donato Bini, Institut des Hautes Etudes Scientifiques (IHES), and IHES

Subjects
gravitational waves, effective-one-body, Element by element, FOS: Physical sciences, alternative theories of gravity, General Relativity and Quantum Cosmology (gr-qc), 01 natural sciences, General Relativity and Quantum Cosmology, spinning bodies, Gravitation, symbols.namesake, 0103 physical sciences, Waveform, 010306 general physics, Spinning, Physics, 010308 nuclear & particles physics, Numerical relativity, Classical mechanics, gravitational waves, General relativity, symbols, Compact form, [PHYS.GRQC]Physics [physics]/General Relativity and Quantum Cosmology [gr-qc], effective-one-body, Hamiltonian (quantum mechanics), Effective one-body formalism
Abstract

TEOBResumS and SEOBNRv4 are the two existing semi-analytical gravitational waveform models for spin-aligned coalescing black hole binaries based on the effective-one-body approach.They are informed by numerical relativity simulations and provide the relative dynamics and waveforms from early inspiral to plunge, merger and ringdown The central building block of each model is the EOB resummed Hamiltonian.The two models implement different Hamiltonians that are both deformations of the Hamiltonian of a test spinning black hole moving around a Kerr black hole.Here we analytically compare, element by element, the two Hamiltonians. In particular: we illustrate that one can introduce a centrifugal radius SEOBNRv4, so to rewrite the Hamiltonian in a more compact form that is analogous to the one of TEOBResumS.The latter centrifugal radius cannot, however, be identified with the one used in TEOBResumS because the two models differ in their ways of incorporating spin effects in their respective deformations of the background Kerr Hamiltonian. We performed extensive comparisons between the energetics corresponding to the two Hamiltonians using gauge-invariant quantities. Finally, as an exploratory investigation, we apply the post-adiabatic approximation to the newly rewritten SEOBNRv4 Hamiltonian, illustrating that it is possible to generate long-inspiral waveforms with negligible computational cost., 23 pages, 13 figures. Submitted to Phys. Rev. D

Published
2019
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177. Shortcomings of Shapiro delay-based tests of the equivalence principle on cosmological scales

Author

Mairi Sakellariadou, Nathan K. Johnson-McDaniel, Olivier Minazzoli, Astrophysique Relativiste Théories Expériences Métrologie Instrumentation Signaux (ARTEMIS), Université Nice Sophia Antipolis (... - 2019) (UNS), COMUE Université Côte d'Azur (2015-2019) (COMUE UCA)-COMUE Université Côte d'Azur (2015-2019) (COMUE UCA)-Institut national des sciences de l'Univers (INSU - CNRS)-Observatoire de la Côte d'Azur, COMUE Université Côte d'Azur (2015-2019) (COMUE UCA)-Université Côte d'Azur (UCA)-Université Côte d'Azur (UCA)-Centre National de la Recherche Scientifique (CNRS), Université Côte d'Azur (UCA)-Université Côte d'Azur (UCA)-Institut national des sciences de l'Univers (INSU - CNRS)-Observatoire de la Côte d'Azur, and Université Côte d'Azur (UCA)-Centre National de la Recherche Scientifique (CNRS)

Subjects
Physics, Newtonian potential, 010308 nuclear & particles physics, General relativity, FOS: Physical sciences, alternative theories of gravity, General Relativity and Quantum Cosmology (gr-qc), 16. Peace & justice, 01 natural sciences, Upper and lower bounds, Shapiro delay, General Relativity and Quantum Cosmology, Gravitational field, 0103 physical sciences, [PHYS.GRQC]Physics [physics]/General Relativity and Quantum Cosmology [gr-qc], Fermi coordinates, Statistical physics, Equivalence principle, 010306 general physics, Divergence (statistics)
Abstract

The "Shapiro delay" experienced by an astronomical messenger traveling through a gravitational field has been used to place constraints on possible deviations from the equivalence principle. The standard Shapiro delay used to obtain these constraints is not itself an observable in general relativity, but is rather obtained by comparing with a fiducial Euclidean distance. There is not a mapping between the constraints obtained in this manner and alternative theories that exhibit equivalence principle violations. However, even assuming that the comparison with the fiducial Euclidean distance is carried out in a way that is useful for some class of alternative theories, we show that the standard calculation of these constraints cannot be applied on cosmological scales, as is often done. Specifically, we find that the Shapiro delay computed in the standard way (taking the Newtonian potential to vanish at infinity) diverges as one includes many remote sources. We use an infinite homogeneous lattice model to illustrate this divergence, and also show how the divergence can be cured by using Fermi coordinates associated with an observer. With this correction, one finds that the Shapiro delay is no longer monotonic with the number of sources. Thus, one cannot compute a conservative lower bound on the Shapiro delay using a subset of the sources of the gravitational field without further assumptions and/or observational input. As an illustration, we compute the Shapiro delay by applying the Fermi coordinate expression to two catalogs of galaxy clusters, illustrating the dependence of the result on the completeness of the catalogue and the mass estimates., 15 pages, 7 figures. Accepted manuscript in Phys. Rev. D

Published
2019
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178. Gravitational-wave amplitudes for compact binaries in eccentric orbits at the third post-Newtonian order: Memory contributions

Author

Y. Boetzel, Chandra Kant Mishra, Guillaume Faye, Philippe Jetzer, Bala R. Iyer, M. Ebersold, University of Zurich, Institut d'Astrophysique de Paris (IAP), and Institut national des sciences de l'Univers (INSU - CNRS)-Sorbonne Université (SU)-Centre National de la Recherche Scientifique (CNRS)

Subjects
Physics::General Physics, Physics and Astronomy (miscellaneous), General relativity, 530 Physics, FOS: Physical sciences, Binary number, alternative theories of gravity, General Relativity and Quantum Cosmology (gr-qc), 10192 Physics Institute, 01 natural sciences, General Relativity and Quantum Cosmology, Gravitation, 0103 physical sciences, Waveform, 3101 Physics and Astronomy (miscellaneous), 010306 general physics, numerical calculations, orbit, Physics, 04.30.Tv, 010308 nuclear & particles physics, Gravitational wave, 04.30.-w, binary: compact, Nonlinear system, Orbit, Classical mechanics, Amplitude, gravitational radiation: emission, [PHYS.GRQC]Physics [physics]/General Relativity and Quantum Cosmology [gr-qc], nonlinear
Abstract

We compute the non-linear memory contributions to the gravitational-wave amplitudes for compact binaries in eccentric orbits at the third post-Newtonian (3PN) order in general relativity. These contributions are hereditary in nature as they are sourced by gravitational waves emitted during the binary's entire dynamical past. Combining these with already available instantaneous and tail contributions we get the complete 3PN accurate gravitational waveform., 22 pages

Published
2019
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179. Uniqueness and energy bounds for static AdS metrics

Author

Yohan Potaux, Piotr T. Chruściel, Gregory J. Galloway, École normale supérieure - Lyon (ENS Lyon), and École normale supérieure de Lyon (ENS de Lyon)

Subjects
High Energy Physics - Theory, Mathematics - Differential Geometry, media_common.quotation_subject, [PHYS.MPHY]Physics [physics]/Mathematical Physics [math-ph], alternative theories of gravity, FOS: Physical sciences, torus, General Relativity and Quantum Cosmology (gr-qc), 01 natural sciences, horizon, General Relativity and Quantum Cosmology, space-time: anti-de Sitter, 0103 physical sciences, FOS: Mathematics, Uniqueness, 010306 general physics, Mathematical physics, media_common, Physics, Toroid, Spacetime, 010308 nuclear & particles physics, [PHYS.HTHE]Physics [physics]/High Energy Physics - Theory [hep-th], Negativity effect, black hole: anti-de Sitter, Infinity, free energy, General relativity, High Energy Physics - Theory (hep-th), Differential Geometry (math.DG), [PHYS.GRQC]Physics [physics]/General Relativity and Quantum Cosmology [gr-qc], Energy (signal processing)
Abstract

International audience; We show that Wang’s proof of uniqueness of anti–de Sitter spacetime can be adapted to provide uniqueness results for strictly static asymptotically locally hyperbolic vacuum metrics with toroidal infinity, and to prove negativity of the free energy E-TS of static asymptotically AdS black holes with toroidal or higher-genus horizons.

Published
2019
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181. Dynamical environments of relativistic binaries: The phenomenon of resonance shifting

Author

Guillaume Rollin, José Lages, Ivan I. Shevchenko, Univers, Transport, Interfaces, Nanostructures, Atmosphère et environnement, Molécules (UMR 6213) (UTINAM), Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS)-Université de Franche-Comté (UFC), and Université Bourgogne Franche-Comté [COMUE] (UBFC)-Université Bourgogne Franche-Comté [COMUE] (UBFC)

Subjects
General relativity, FOS: Physical sciences, alternative theories of gravity, Binary number, Inverse, General Relativity and Quantum Cosmology (gr-qc), Lyapunov exponent, 01 natural sciences, General Relativity and Quantum Cosmology, symbols.namesake, 0103 physical sciences, 010306 general physics, Earth and Planetary Astrophysics (astro-ph.EP), Physics, 010308 nuclear & particles physics, Plane (geometry), Nonlinear Sciences - Chaotic Dynamics, [PHYS.PHYS.PHYS-GEN-PH]Physics [physics]/Physics [physics]/General Physics [physics.gen-ph], Quantum electrodynamics, [PHYS.GRQC]Physics [physics]/General Relativity and Quantum Cosmology [gr-qc], symbols, Chaotic Dynamics (nlin.CD), Test particle, Circumbinary planet, [PHYS.ASTR]Physics [physics]/Astrophysics [astro-ph], Schwarzschild radius, Astrophysics - Earth and Planetary Astrophysics
Abstract

In this article, we explore both numerically and analytically how the dynamical environments of mildly relativistic binaries evolve with increasing the general relativity factor $\gamma$ (the normalized inverse of the binary size measured in the units of the gravitational radius corresponding to the total mass of the system). Analytically, we reveal a phenomenon of the relativistic shifting of mean-motion resonances: on increasing $\gamma$, the resonances between the test particle and the central binary shift, due to the relativistic variation of the mean motions of the primary and secondary binaries and the relativistic advance of the tertiary's pericenter. To exhibit the circumbinary dynamics globally, we numerically integrate equations of the circumbinary motion of a test particle, and construct relevant scans of the maximum Lyapunov exponents and stability diagrams in the "pericentric distance -- eccentricity" plane of initial conditions. In these scans and diagrams, regular and chaotic domains are identified straightforwardly. Our analytical and numerical estimates of the shift size are in a good agreement. Prospects for identification of the revealed effect in astronomical observations are discussed., Comment: 22 pages, 6 figures. Accepted for publication in Physical Review D

Published
2019
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182. New method to generate exact scalar-tensor solutions

Author

Bertrand Chauvineau, Université Côte d’Azur, Observatoire de la Côte d’Azur, CNRS, Laboratoire Lagrange, Bd de l’Observatoire, CS 34229, 06304 Nice, Joseph Louis LAGRANGE (LAGRANGE), Université Nice Sophia Antipolis (... - 2019) (UNS), Université Côte d'Azur (UCA)-Université Côte d'Azur (UCA)-Observatoire de la Côte d'Azur, Université Côte d'Azur (UCA)-Centre National de la Recherche Scientifique (CNRS), Université Côte d'Azur (UCA)-Université Nice Sophia Antipolis (... - 2019) (UNS), COMUE Université Côte d'Azur (2015-2019) (COMUE UCA)-COMUE Université Côte d'Azur (2015-2019) (COMUE UCA)-Observatoire de la Côte d'Azur, and COMUE Université Côte d'Azur (2015-2019) (COMUE UCA)-Université Côte d'Azur (UCA)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS)

Subjects
Angular momentum, family, General relativity, Kerr metric, Scalar (mathematics), alternative theories of gravity, Ricci, angular momentum, Brans-Dicke model, rotation, symmetry: axial, 01 natural sciences, General Relativity and Quantum Cosmology, Singularity, 0103 physical sciences, structure, 010306 general physics, ComputingMilieux_MISCELLANEOUS, Mathematical physics, Physics, charge: scalar, space-time: vacuum state, 010308 nuclear & particles physics, metric: Kerr, singularity, field theory: scalar, Method of undetermined coefficients, [SDU]Sciences of the Universe [physics], [PHYS.GRQC]Physics [physics]/General Relativity and Quantum Cosmology [gr-qc], Axial symmetry
Abstract

A new method is proposed, that establishes a one to one correspondance between the whole set of static axially symmetric vacuum general relativity solutions and a specific class of stationary axially symmetric scalar-Einstein (${R}_{ab}={\ensuremath{\partial}}_{a}\ensuremath{\varphi}{\ensuremath{\partial}}_{b}\ensuremath{\varphi}$) solutions for any mass and angular momentum. The method explicitly takes advantage of the Kerr metric Ricci flatness. This also results in a class of stationary axially symmetric vacuum, ie Kerrlike, Brans-Dicke solutions. A particular solution, that is asymptotically flat, is more closely considered. It converges to Kerr for a vanishing scalar charge, but fails to converge to the Fisher-Janis-Newman-Winicour solution for a vanishing ``rotation parameter.'' This solution exhibits a set of singular points, with a naked subset having a ringlike structure.

Published
2019
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183. All-sky search for continuous gravitational waves from isolated neutron stars using Advanced LIGO O2 data

Author

P. G. Murray, Fabien Kéfélian, J. H. Hough, P. W. F. Forsyth, S. R. Thondapu, J. R. Palamos, Michele Zanolin, D. B. Kozak, T. J. Massinger, T. Vo, L. Xiao, D. Stocks, V. Kalogera, C. Vorvick, G. D. Hammond, Javed Rana, Martin Obergaulinger, Nicolas Sanchis-Gual, P. Weßels, L. Kuo, H. Yamamoto, J. C. Driggers, A. Schönbeck, B. Rajbhandari, Daniel Wysocki, J. Prasad, Steven Bloemen, Zhihui Du, Jonathan R. Gair, G. Ciani, N. A. Lockerbie, Carlos O. Lousto, C. North, Thomas Dent, P. Corban, A. Parida, S. S. Eikenberry, James Whelan, P. Ajith, Jordan Camp, Rosa Poggiani, N. V. Keerthana, Marco Romanelli, V. Frey, A. K. Mehta, P. Fulda, T. Hardwick, D. Steinmeyer, S. Farinon, A. Pele, G. Koekoek, P. Raffai, A. J. Weinstein, M. Bawaj, J. Hanks, G. D. O'Dea, S. E. Barclay, J. L. Willis, M. Eisenmann, Ofek Birnholtz, Charalampos Markakis, Bruno Giacomazzo, M. P. Ross, T. B. Edo, Nicholas Demos, J. D. Lough, Soma Mukherjee, J. Suresh, Maximiliano Isi, B. D. Lackey, Miftar Ganija, D. Huet, S. H. Huttner, Samuele Cortese, M. Haney, B. L. Swinkels, M. Croquette, S. Sitmukhambetov, Eric Howell, S. Leavey, Hai-Ping Cheng, A. Iess, S. Penn, G. L. Mansell, Sebastiano Bernuzzi, O. Halim, F. Cleva, Andrew Melatos, M. Lorenzini, V. Boschi, R. J. G. Jonker, Jay D. Tasson, F. Lin, Tania Regimbau, Piotr Jaranowski, S. B. Anderson, Archisman Ghosh, C. C. Yancey, L. K. Nuttall, O. Dorosh, R. Macas, G. Billingsley, S. Macfoy, T. A. Callister, N. Kijbunchoo, Mairi Sakellariadou, J. H. Briggs, Mark Hannam, F. Thies, G. Greco, D. Moraru, Gianpietro Cagnoli, A. C. Green, E. M. Gretarsson, Ying Guo, D. Beniwal, Peter Fritschel, Wenxiao Wang, Tim Dietrich, Charlie Hoy, G. Rutins, Tanja Hinderer, A. Strunk, K. W. Tsang, P. Booker, L. Trozzo, Albert Lazzarini, R. Pedurand, Benno Willke, C. D. Booth, Giuseppe Intini, M. Landry, L. Di Fiore, B. Mours, C. Austin, Graham Woan, Robert L. Byer, W. G. Anderson, P. Grassia, Kipp Cannon, M. Steinke, Stuart Reid, F. J. Hayes, A. Samajdar, M. Masso-Reid, J. Jiang, M. Drago, Guenakh Mitselmakher, Jade Powell, V. Mangano, Sheelu Abraham, P. T.H. Pang, Fausto Acernese, S. Appert, Y. Setyawati, A. Giazotto, V. Dattilo, Stefan Hild, Y. Ma, C. Cahillane, J. Hennig, G. Cella, K. Rao, Podila Satya Venkata Narasimha Sharma, D. M. Wilken, B. P. Abbott, E. K. Gustafson, P. Shawhan, I. Ferrante, Chris A. Collins, R. Gray, S. H. R. Yuen, O. de Varona, Rico K. L. Lo, P. Charlton, C. Gray, G. H. Ogin, J. Liu, H. K. Gulati, David H. Reitze, Rahul Kashyap, B. A. Boom, A. M. Sergeev, Jacob Scheuer, M. Rakhmanov, Zachariah B. Etienne, Jennifer Watchi, G. Pagano, J.-P. Zendri, Bernard F. Schutz, Li Ju, Daniel A. Shaddock, Brittany Kamai, M. Barsuglia, K. Chatziioannou, T. J. Shaffer, Y. Bouffanais, C. V. Kalaghatgi, J. Hanson, Kejia Lee, A. M. Holgado, K. G. Arun, S. V. Angelova, M. Fitz-Axen, P. Bacon, Daniel E. Holz, M. Mantovani, Hyang Woon Lee, A. Grant, Debnandini Mukherjee, S. Doravari, G. Weldon, Christopher P. L. Berry, A. D. Silva, Sanjay Kumar, Jianfang Wang, T. P. Downes, Sascha Husa, G. Venugopalan, D.B. DeBra, A. K. Zadrożny, H. Estelles, G. Mo, V. Sequino, C. J. Richardson, Tenglin Li, C. Buy, Yuri Levin, I. Kowalska, D. Estevez, Rana X. Adhikari, F. Donovan, S. C. Tait, Alejandro Torres-Forné, K. Siellez, T. Etzel, A. Chiummo, A. Miller, V. Gayathri, S. Walsh, Miriam Cabero, Alessandra Buonanno, A. Allocca, Hang Yu, S. Vass, P. Puppo, Zifan Zhou, N. Letendre, S. Mastrogiovanni, L. E. Sanchez, R. K. Lanza, P. Dupej, R. Coyne, P. Ciecielag, R. Kennedy, C. S. Unnikrishnan, I. A. Bilenko, L. Haegel, David J. Ottaway, M. Tse, J. Derby, D. M. Macleod, K. A. Thorne, Isabel Cordero-Carrión, M. Brinkmann, D. Buskulic, M. H. Wimmer, A. Effler, L. Zhang, Fabrice Matichard, G. Giordano, J. H. Klika, O. Sauter, A. Cirone, Hyun Lee, Enrico Calloni, Eric B. Flynn, M. Pedraza, G. Traylor, B. Irwin, Marie-Anne Bizouard, J. N. Leviton, S. Márka, D. Pascucci, S. Antier, Samaya Nissanke, B. K. Berger, P. J. Veitch, Geoffrey Lovelace, J. Neilson, R. Metzdorff, Gabrielle Allen, Luca Gammaitoni, J.-M. Isac, M. Chan, O. J. Piccinni, M. Boer, J. B. Kanner, E. A. Huerta, B. Gateley, Nikhil Sarin, C. F. Da Silva Costa, D. Lumaca, Thomas Corbitt, C. Bradaschia, Aaron Buikema, L. Salconi, C. A. Costa, C. C. Wipf, S. A. Usman, Roman Schnabel, Matthew Evans, E. K. Wessel, S. E. Dwyer, David Keitel, B. Patricelli, E. Capocasa, Christian Pedersen, L. Pinard, V. Tiwari, Lloyd Paul Aiello, N. V. Krishnendu, P. Kumar, C. Affeldt, N. Sennett, B. Lantz, F. Cavalier, R. Taylor, Kenneth A. Strain, Jimin George, P. T. Baker, R. Goetz, J. Calderón Bustillo, P. A. Altin, E. J. King, H. Fong, J. E. Brau, A. A. van Veggel, Bala R. Iyer, M. Merzougui, B. R. Hall, G. Vedovato, S. J. Cooper, Nergis Mavalvala, Jerome Degallaix, D. S. Wu, Margaret Millhouse, B. C. Pant, C. Casentini, F. Robinet, E. Bonilla, Q. Chu, M. Bejger, M. Sieniawska, K. Mason, Brynmor Haskell, Tarun Souradeep, M. Yvert, R. M. S. Schofield, C. L. Romel, Efim A. Khazanov, G. Ballardin, M. J. Cowart, Gregory Ashton, K. Chakravarti, S. D'Antonio, A. L. Stuver, D. Barker, B. Sassolas, Gregorio Carullo, S. McCormick, A. Lartaux-Vollard, A. Ain, R. J. Trudeau, M. Oliver, W. Z. Korth, Sebastian Khan, B. C. Barish, M. K. M. Bader, C. Fee, A. K. Srivastava, A. E. Pace, Kazuhiro Agatsuma, R. Inta, F. Marion, Frank Ohme, M. Tonelli, Benjamin J. Owen, M. A. Okada, Shubhanshu Tiwari, Fabio Marchesoni, Torrey Cullen, D. Tuyenbayev, T. Zhang, S. G. Gaonkar, Thibaut Jacqmin, G. Wang, J. F. J. van den Brand, S. Klimenko, Suvadeep Bose, E. Cesarini, L. Naticchioni, R. Gouaty, E. C. Ferreira, Salvatore Vitale, Sanjeev Dhurandhar, Sourav Ghosh, D. C. Vander-Hyde, A. Brillet, O. Chaibi, Imre Bartos, A. Basti, Ryan N. Lang, John A. Clark, Ben Farr, S. Sunil, M. Tacca, Martin Hendry, Cecilio García-Quirós, S. Hochheim, S. Frasca, S. Ponrathnam, S. Mitra, F. Garufi, M. Standke, D. J. McManus, Otto A. Hannuksela, C. I. Torrie, N. A. 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S, Kang, G, Kanner, J, Kapadia, S, Karki, S, Karvinen, K, Kashyap, R, Kasprzack, M, Katsanevas, S, Katsavounidis, E, Katzman, W, Kaufer, S, Kawabe, K, Keerthana, N, Kéfélian, F, Keitel, D, Kennedy, R, Key, J, Khalili, F, Khan, H, Khan, I, Khan, S, Khan, Z, Khazanov, E, Khursheed, M, Kijbunchoo, N, Kim, C, Kim, J, Kim, K, Kim, W, Kim, Y, Kimball, C, King, E, King, P, Kinley-Hanlon, M, Kirchhoff, R, Kissel, J, Kleybolte, L, Klika, J, Klimenko, S, Knowles, T, Koch, P, Koehlenbeck, S, Koekoek, G, Koley, S, Kondrashov, V, Kontos, A, Koper, N, Korobko, M, Korth, W, Kowalska, I, Kozak, D, Kringel, V, Krishnendu, N, Królak, A, Kuehn, G, Kumar, A, Kumar, P, Kumar, R, Kumar, S, Kuo, L, Kutynia, A, Kwang, S, Lackey, B, Lai, K, Lam, T, Landry, M, Lane, B, Lang, R, Lange, J, Lantz, B, Lanza, R, Lartaux-Vollard, A, Lasky, P, Laxen, M, Lazzarini, A, Lazzaro, C, Leaci, P, Leavey, S, Lecoeuche, Y, Lee, C, Lee, H, Lee, J, Lee, K, Lehmann, J, Lenon, A, Leroy, N, Letendre, N, Levin, Y, Leviton, J, Li, J, Li, K, Li, T, Li, X, Lin, F, Linde, F, Linker, S, Littenberg, T, Liu, J, Liu, X, Lo, R, Lockerbie, N, London, L, Longo, A, Lorenzini, M, Loriette, V, Lormand, M, Losurdo, G, Lough, J, Lousto, C, Lovelace, G, Lower, M, Lück, H, Lumaca, D, Lundgren, A, Lynch, R, Ma, Y, Macas, R, Macfoy, S, Macinnis, M, Macleod, D, Macquet, A, Magaña-Sandoval, F, Magaña Zertuche, L, Magee, R, Majorana, E, Maksimovic, I, Malik, A, Man, N, Mandic, V, Mangano, V, Mansell, G, Manske, M, Mantovani, M, Marchesoni, F, Marion, F, Márka, S, Márka, Z, Markakis, C, Markosyan, A, Markowitz, A, Maros, E, Marquina, A, Marsat, S, Martelli, F, Martin, I, Martin, R, Martynov, D, Mason, K, Massera, E, Masserot, A, Massinger, T, Masso-Reid, M, Mastrogiovanni, S, Matas, A, Matichard, F, Matone, L, Mavalvala, N, Mazumder, N, Mccann, J, Mccarthy, R, Mcclelland, D, Mccormick, S, Mcculler, L, Mcguire, S, Mciver, J, Mcmanus, D, Mcrae, T, Mcwilliams, S, Meacher, D, Meadors, G, Mehmet, M, Mehta, A, Meidam, J, Melatos, A, Mendell, 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Rei, L, Reid, S, Reitze, D, Ren, W, Ricci, F, Richardson, C, Richardson, J, Ricker, P, Riles, K, Rizzo, M, Robertson, N, Robie, R, Robinet, F, Rocchi, A, Rolland, L, Rollins, J, Roma, V, Romanelli, M, Romano, R, Romel, C, Romie, J, Rose, K, Rosińska, D, Rosofsky, S, Ross, M, Rowan, S, Rüdiger, A, Ruggi, P, Rutins, G, Ryan, K, Sachdev, S, Sadecki, T, Sakellariadou, M, Salconi, L, Saleem, M, Samajdar, A, Sammut, L, Sanchez, E, Sanchez, L, Sanchis-Gual, N, Sandberg, V, Sanders, J, Santiago, K, Sarin, N, Sassolas, B, Sathyaprakash, B, Saulson, P, Sauter, O, Savage, R, Schale, P, Scheel, M, Scheuer, J, Schmidt, P, Schnabel, R, Schofield, R, Schönbeck, A, Schreiber, E, Schulte, B, Schutz, B, Schwalbe, S, Scott, J, Scott, S, Seidel, E, Sellers, D, Sengupta, A, Sennett, N, Sentenac, D, Sequino, V, Sergeev, A, Setyawati, Y, Shaddock, D, Shaffer, T, Shahriar, M, Shaner, M, Shao, L, Sharma, P, Shawhan, P, Shen, H, Shink, R, Shoemaker, D, Shyamsundar, S, Siellez, K, Sieniawska, M, Sigg, D, Silva, 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Unnikrishnan, C, Urban, A, Usman, S, Vahlbruch, H, Vajente, G, Valdes, G, van Bakel, N, van Beuzekom, M, van den Brand, J, Van Den Broeck, C, Vander-Hyde, D, van Heijningen, J, van der Schaaf, L, van Veggel, A, Vardaro, M, Varma, V, Vass, S, Vasúth, M, Vecchio, A, Vedovato, G, Veitch, J, Veitch, P, Venkateswara, K, Venugopalan, G, Verkindt, D, Vetrano, F, Viceré, A, Viets, A, Vine, D, Vinet, J, Vitale, S, Vo, T, Vocca, H, Vorvick, C, Vyatchanin, S, Wade, A, Wade, L, Wade, M, Walet, R, Walker, M, Wallace, L, Walsh, S, Wang, G, Wang, H, Wang, J, Wang, W, Wang, Y, Ward, R, Warden, Z, Warner, J, Was, M, Watchi, J, Weaver, B, Wei, L, Weinert, M, Weinstein, A, Weiss, R, Weldon, G, Wellmann, F, Wen, L, Wessel, E, Weßels, P, Westhouse, J, Wette, K, Whelan, J, Whiting, B, Whittle, C, Wilken, D, Williams, D, Williamson, A, Willis, J, Willke, B, Wimmer, M, Winkler, W, Wipf, C, Wittel, H, Woan, G, Woehler, J, Wofford, J, Worden, J, Wright, J, Wu, D, Wysocki, D, Xiao, L, Yamamoto, H, Yancey, C, 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P., Abbott, R., Abbott, T. D., Abraham, S., Acernese, F., Ackley, K., Adams, C., Adhikari, R. X., Adya, V. B., Affeldt, C., Agathos, M., Agatsuma, K., Aggarwal, N., Aguiar, O. D., Aiello, L., Ain, A., Ajith, P., Allen, G., Allocca, A., Aloy, M. A., Altin, P. A., Amato, A., Ananyeva, A., Anderson, S. B., Anderson, W. G., Angelova, S. V., Antier, S., Appert, S., Arai, K., Araya, M. C., Areeda, J. S., Arene, M., Arnaud, N., Arun, K. G., Ascenzi, S., Ashton, G., Aston, S. M., Astone, P., Aubin, F., Aufmuth, P., Aultoneal, K., Austin, C., Avendano, V., Avila-Alvarez, A., Babak, S., Bacon, P., Badaracco, F., Bader, M. K. M., Bae, S., Baker, P. T., Baldaccini, F., Ballardin, G., Ballmer, S. W., Banagiri, S., Barayoga, J. C., Barclay, S. E., Barish, B. C., Barker, D., Barkett, K., Barnum, S., Barone, F., Barr, B., Barsotti, L., Barsuglia, M., Barta, D., Bartlett, J., Bartos, I., Bassiri, R., Basti, A., Bawaj, M., Bayley, J. C., Bazzan, M., Becsy, B., Bejger, M., Belahcene, I., Bell, A. S., Beniwal, D., Berger, B. K., Bergmann, G., Bernuzzi, S., Bero, J. J., Berry, C. P. L., Bersanetti, D., Bertolini, A., Betzwieser, J., Bhandare, R., Bidler, J., Bilenko, I. A., Bilgili, S. A., Billingsley, G., Birch, J., Birney, R., Birnholtz, O., Biscans, S., Biscoveanu, S., Bisht, A., Bitossi, M., Bizouard, M. A., Blackburn, J. K., Blair, C. D., Blair, D. G., Blair, R. M., Bloemen, S., Bode, N., Boer, M., Boetzel, Y., Bogaert, G., Bondu, F., Bonilla, E., Bonnand, R., Booker, P., Boom, B. A., Booth, C. D., Bork, R., Boschi, V., Bose, S., Bossie, K., Bossilkov, V., Bosveld, J., Bouffanais, Y., Bozzi, A., Bradaschia, C., Brady, P. R., Bramley, A., Branchesi, M., Brau, J. E., Briant, T., Briggs, J. H., Brighenti, F., Brillet, A., Brinkmann, M., Brisson, V., Brockill, P., Brooks, A. F., Brown, D. D., Brunett, S., Buikema, A., Bulik, T., Bulten, H. J., Buonanno, A., Buskulic, D., Buy, C., Byer, R. L., Cabero, M., Cadonati, L., Cagnoli, G., Cahillane, C., Calderon Bustillo, J., Callister, T. A., Calloni, E., Camp, J. B., Campbell, W. A., Cannon, K. C., Cao, H., Cao, J., Capocasa, E., Carbognani, F., Caride, S., Carney, M. F., Carullo, G., Casanueva Diaz, J., Casentini, C., Caudill, S., Cavaglia, M., Cavalier, F., Cavalieri, R., Cella, G., Cerda-Duran, P., Cerretani, G., Cesarini, E., Chaibi, O., Chakravarti, K., Chamberlin, S. J., Chan, M., Chao, S., Charlton, P., Chase, E. A., Chassande-Mottin, E., Chatterjee, D., Chaturvedi, M., Chatziioannou, K., Cheeseboro, B. D., Chen, H. Y., Chen, X., Chen, Y., Cheng, H. -P., Cheong, C. K., Chia, H. Y., Chincarini, A., Chiummo, A., Cho, G., Cho, H. S., Cho, M., Christensen, N., Chu, Q., Chua, S., Chung, K. W., Chung, S., Ciani, G., Ciecielag, P., Ciobanu, A. A., Ciolfi, R., Cipriano, F., Cirone, A., Clara, F., Clark, J. A., Clearwater, P., Cleva, F., Cocchieri, C., Coccia, E., Cohadon, P. -F., Cohen, D., Colgan, R., Colleoni, M., Collette, C. G., Collins, C., Cominsky, L. R., Constancio, M., Conti, L., Cooper, S. J., Corban, P., Corbitt, T. R., Cordero-Carrion, I., Corley, K. R., Cornish, N., Corsi, A., Cortese, S., Costa, C. A., Cotesta, R., Coughlin, M. W., Coughlin, S. B., Coulon, J. -P., Countryman, S. T., Couvares, P., Covas, P. B., Cowan, E. E., Coward, D. M., Cowart, M. J., Coyne, D. C., Coyne, R., Creighton, J. D. E., Creighton, T. D., Cripe, J., Croquette, M., Crowder, S. G., Cullen, T. J., Cumming, A., Cunningham, L., Cuoco, E., Dal Canton, T., Dalya, G., Danilishin, S. L., D'Antonio, S., Danzmann, K., Dasgupta, A., Da Silva Costa, C. F., Datrier, L. E. H., Dattilo, V., Dave, I., Davier, M., Davis, D., Daw, E. J., Debra, D., Deenadayalan, M., Degallaix, J., De Laurentis, M., Deleglise, S., Del Pozzo, W., Demarchi, L. M., Demos, N., Dent, T., De Pietri, R., Derby, J., De Rosa, R., De Rossi, C., Desalvo, R., De Varona, O., Dhurandhar, S., Diaz, M. C., Dietrich, T., Di Fiore, L., Di Giovanni, M., Di Girolamo, T., Di Lieto, A., Ding, B., Di Pace, S., Di Palma, I., Di Renzo, F., Dmitriev, A., Doctor, Z., Donovan, F., Dooley, K. L., Doravari, S., Dorosh, O., Dorrington, I., Downes, T. P., Drago, M., Driggers, J. C., Du, Z., Ducoin, J. -G., Dupej, P., Dwyer, S. E., Easter, P. J., Edo, T. B., Edwards, M. C., Effler, A., Ehrens, P., Eichholz, J., Eikenberry, S. S., Eisenmann, M., Eisenstein, R. A., Essick, R. C., Estelles, H., Estevez, D., Etienne, Z. B., Etzel, T., Evans, M., Evans, T. M., Fafone, V., Fair, H., Fairhurst, S., Fan, X., Farinon, S., Farr, B., Farr, W. M., Fauchon-Jones, E. J., Favata, M., Fays, M., Fazio, M., Fee, C., Feicht, J., Fejer, M. M., Feng, F., Fernandez-Galiana, A., Ferrante, I., Ferreira, E. C., Ferreira, T. 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A., Huet, D., Hughey, B., Hulko, M., Husa, S., Huttner, S. H., Huynh-Dinh, T., Idzkowski, B., Iess, A., Ingram, C., Inta, R., Intini, G., Irwin, B., Isa, H. N., Isac, J. -M., Isi, M., Iyer, B. R., Izumi, K., Jacqmin, T., Jadhav, S. J., Jani, K., Janthalur, N. N., Jaranowski, P., Jenkins, A. C., Jiang, J., Johnson, D. S., Jones, A. W., Jones, D. I., Jones, R., Jonker, R. J. G., Ju, L., Junker, J., Kalaghatgi, C. V., Kalogera, V., Kamai, B., Kandhasamy, S., Kang, G., Kanner, J. B., Kapadia, S. J., Karki, S., Karvinen, K. S., Kashyap, R., Kasprzack, M., Katsanevas, S., Katsavounidis, E., Katzman, W., Kaufer, S., Kawabe, K., Keerthana, N. V., Kefelian, F., Keitel, D., Kennedy, R., Key, J. S., Khalili, F. Y., Khan, H., Khan, I., Khan, S., Khan, Z., Khazanov, E. A., Khursheed, M., Kijbunchoo, N., Kim, C., Kim, J. C., Kim, K., Kim, W., Kim, W. S., Kim, Y. -M., Kimball, C., King, E. J., King, P. J., Kinley-Hanlon, M., Kirchhoff, R., Kissel, J. S., Kleybolte, L., Klika, J. 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Ferreira, Ta, Fishner, Jm, Gulati, Hk, Hayes, Fj, Vivanco, Fh, Holgado, Am, Holland, Na, Hoy, Cg, Jadhav, Sj, Janthalur, Nn, Jones, Di, Keerthana, Nv, Kefelian, F, Khalili, Fy, Khazanov, Ea, Kim, Jc, Kim, Ym, King, Ej, King, Pj, Klika, Jh, Knowles, Td, Koehlenbeck, Sm, Korth, Wz, Kozak, Db, Krolak, A, Lackey, Bd, Lai, Kh, Lam, Tl, Lane, Bb, Lang, Rn, Lanza, Rk, Lasky, Pd, Lecoeuche, Yk, Lee, Ch, Lee, Hk, Lee, Hm, Lee, Hw, Li, Kjl, Li, Tgf, Linker, Sd, Littenberg, Tb, Lo, Rkl, Lockerbie, Na, London, Lt, Lough, Jd, Lousto, Co, Lower, Me, Luck, H, Lundgren, Ap, Macleod, Dm, Magana-Sandoval, F, Zertuche, Lm, Magee, Rm, Mansell, Gl, Marka, S, Marka, Z, Martin, Iw, Martin, Rm, Martynov, Dv, Massinger, Tj, Mccann, Jj, Mcclelland, De, Mcguire, Sc, Mcmanus, Dj, Mcwilliams, St, Meadors, Gd, Mehta, Ak, Mercer, Ra, Merilh, El, Meyers, Pm, Mikhailov, Ee, Miller, Al, Mills, Jc, Milovich-Goff, Mc, Mitrofanov, Vp, Mohapatra, Srp, Moore, Cj, Mow-Lowry, Cm, Muniz, Ea, Murray, Pg, Nayak, Rk, Nelson, Tjn, Ng, Ky, Nuttall, Lk, Obrien, Bd, Odea, Gd, Ogin, Gh, Oh, Jj, Oh, Sh, Okada, Ma, Oram, Rj, Oreilly, B, Ormiston, Rg, Ortega, Lf, Oshaughnessy, R, Ottaway, Dj, Owen, Bj, Pace, Ae, Page, Ma, Pai, Sa, Palamos, Jr, Pan, Hw, Pang, Pth, Pant, Bc, Pearlstone, Bl, Perez, Cj, Pfeiffer, Hp, Piccinni, Oj, Pong, Dyt, Porter, Ek, Prajapati, Ak, Prodi, Ga, Prokhorov, Lg, Purrer, M, Quinonez, Pj, Quintero, Ea, Raab, Fj, Ramirez, Ke, Reitze, Dh, Richardson, Cj, Richardson, Jw, Ricker, Pm, Robertson, Na, Rollins, Jg, Roma, Vj, Romel, Cl, Romie, Jh, Rosinska, D, Rosofsky, Sg, Ross, Mp, Rudiger, A, Sanchez, Ej, Sanchez, Le, Sanders, Jr, Santiago, Ka, Saulson, Pr, Savage, Rl, Schofield, Rm, Schonbeck, A, Schulte, Bw, Schutz, Bf, Schwalbe, Sg, Scott, Sm, Shaddock, Da, Shaner, Mb, Shoemaker, Dh, Shoemaker, Dm, Silva, Ad, Singer, Lp, Sintes, Am, Slagmolen, Bjj, Slaven-Blair, Tj, Smith, Jr, Smith, Rje, Son, Ej, Spencer, Ap, Srivastava, Ak, Steer, Da, Stevenson, Sp, Stops, Dj, Strain, Ka, Strigin, Se, Stuver, Al, Summerscales, Tz, Sutton, Pj, Swinkels, Bl, Szczepanczyk, Mj, Tait, Sc, Tanner, Db, Tapai, M, Tasson, Jd, Thondapu, Sr, Thorne, Ka, Torres-Forne, A, Torrie, Ci, Toyra, D, Tringali, Mc, Tsang, Kw, Urban, Al, Usman, Sa, van den Brand, Jfj, Vander-Hyde, Dc, van Heijningen, Jv, van Der Schaaf, L, van Veggel, Aa, Vasuth, M, Veitch, Pj, Vicere, A, Viets, Ad, Vine, Dj, Vinet, Jy, Vyatchanin, Sp, Wade, Ar, Wade, Le, Wang, Jz, Wang, Wh, Wang, Yf, Ward, Rl, Warden, Za, Wei, Lw, Weinstein, Aj, Wessel, Ek, Weels, P, Westhouse, Jw, Whelan, Jt, Whiting, Bf, Wilken, Dm, Williamson, Ar, Willis, Jl, Wimmer, Mh, Wipf, Cc, Wofford, Jk, Wright, Jl, Wysocki, Dm, Yancey, Cc, Yap, Mj, Yeeles, Dw, Yu, Hc, Yuen, Shr, Zadrozny, Ak, Zendri, Jp, Zhu, Xj, and Zucker, Me

Subjects
Astronomy, Astrophysics, Rotation, 01 natural sciences, rotation, Gravitation, Cosmology & Astrophysics, General Relativity and Quantum Cosmology, Physics, Particles & Fields, continuous gravitational wave, LIGO, neutron star, GeneralLiterature_REFERENCE(e.g.,dictionaries,encyclopedias,glossaries), media_common, High Energy Astrophysical Phenomena (astro-ph.HE), Settore FIS/01, Physics, astro-ph.HE, Physical Systems, Amplitude, General relativity, gravitational waves, Physical Sciences, [PHYS.GRQC]Physics [physics]/General Relativity and Quantum Cosmology [gr-qc], Gravitational wave detection, Astrophysics - High Energy Astrophysical Phenomena, continuous gravitational waves, Advanced LIGO, asymmetry, Gravitation, Neutron stars & pulsars, Frequency band, media_common.quotation_subject, gr-qc, FOS: Physical sciences, alternative theories of gravity, General Relativity and Quantum Cosmology (gr-qc), Astronomy & Astrophysics, Gravitational waves, 0103 physical sciences, ddc:530, 010306 general physics, gravitational radiation: frequency, STFC, gravitational waves,neutron stars, Gravitational wave sources, Science & Technology, Gravitational wave sources, Gravitational waves, Physical Systems, Neutron stars and pulsars, Gravitational wave detection, 010308 nuclear & particles physics, Gravitational wave, RCUK, Gravitational Wave Physics, Neutron star, Sky, Neutron stars and pulsars, Dewey Decimal Classification::500 | Naturwissenschaften::530 | Physik, [PHYS.ASTR]Physics [physics]/Astrophysics [astro-ph]
Abstract

We present results of an all-sky search for continuous gravitational waves (CWs), which can be produced by fast-spinning neutron stars with an asymmetry around their rotation axis, using data from the second observing run of the Advanced LIGO detectors. We employ three different semi-coherent methods ($\textit{FrequencyHough}$, $\textit{SkyHough}$, and $\textit{Time-Domain $\mathcal{F}$-statistic}$) to search in a gravitational-wave frequency band from 20 to 1922 Hz and a first frequency derivative from $-1\times10^{-8}$ to $2\times10^{-9}$ Hz/s. None of these searches has found clear evidence for a CW signal, so we present upper limits on the gravitational-wave strain amplitude $h_0$ (the lowest upper limit on $h_0$ is $1.7\times10^{-25}$ in the 123-124 Hz region) and discuss the astrophysical implications of this result. This is the most sensitive search ever performed over the broad range of parameters explored in this study.

Published
2019
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184. Environment dependence of the growth of the most massive objects in the Universe

Author

Jan J. Ostrowski, Krzysztof Bolejko, Centre de Recherche Astrophysique de Lyon (CRAL), École normale supérieure de Lyon (ENS de Lyon)-Université Claude Bernard Lyon 1 (UCBL), Université de Lyon-Université de Lyon-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS), Centre National de la Recherche Scientifique (CNRS)-Institut national des sciences de l'Univers (INSU - CNRS)-Université Claude Bernard Lyon 1 (UCBL), Université de Lyon-Université de Lyon-École normale supérieure - Lyon (ENS Lyon), École normale supérieure - Lyon (ENS Lyon)-Université Claude Bernard Lyon 1 (UCBL), and Université de Lyon-Université de Lyon-Centre National de la Recherche Scientifique (CNRS)-Institut national des sciences de l'Univers (INSU - CNRS)

Subjects
Physics, Cosmology and Nongalactic Astrophysics (astro-ph.CO), 010308 nuclear & particles physics, media_common.quotation_subject, FOS: Physical sciences, alternative theories of gravity, Astrophysics::Cosmology and Extragalactic Astrophysics, Function (mathematics), Cosmological model, Curvature, 01 natural sciences, Measure (mathematics), Universe, Cosmology, Amplitude, General relativity, 0103 physical sciences, Spatial homogeneity, [PHYS.ASTR]Physics [physics]/Astrophysics [astro-ph], 010303 astronomy & astrophysics, Astrophysics - Cosmology and Nongalactic Astrophysics, media_common, Mathematical physics
Abstract

This paper investigates the growth of the most massive cosmological objects. We utilize the Simsilun simulation, which is based on the approximation of the silent universe. In the limit of spatial homogeneity and isotropy the silent universes reduce to the standard FLRW models. We show that within the approximation of the silent universe the formation of the most massive cosmological objects differs from the standard background-dependent approaches. For objects with masses above $10^{15} M_\odot$ the effect of spatial curvature (overdense regions are characterized by positive spatial curvature) leads to measurable effects. The effect is analogous to the effect that the background cosmological model has on the formation of these objects (i.e. the higher matter density and spatial curvature the faster the growth of cosmic structures). We measure this by the means of the mass function and show that the mass function obtained from the Simsilun simulation has a higher amplitude at the high-mass end compared to standard mass function such as the Press-Schechter or the Tinker mass function. For comparison, we find that the expected mass of most massive objects using the Tinker mass function is $4.4^{+0.8}_{-0.6} \, \times 10^{15} M_\odot$, whereas for the Simsilun simulation is $6.3^{+1.0}_{-0.8} \, \times 10^{15} M_\odot$. We conclude that the nonlinear relativistic effects could affect the formation of the most massive cosmological objects, leading to a relativistic environment-dependence of the growth rate of the most massive clusters., 9 pages, 6 figures

Published
2019
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185. Regge pole description of scattering of gravitational waves by a Schwarzschild black hole

Author

Antoine Folacci, Mohamed Ould El Hadj, and Université Pascal Paoli (UPP)

Subjects
High Energy Physics - Theory, Angular momentum, approximation: semiclassical, Scalar (mathematics), Semiclassical physics, FOS: Physical sciences, alternative theories of gravity, General Relativity and Quantum Cosmology (gr-qc), 01 natural sciences, Electromagnetic radiation, frequency: high, General Relativity and Quantum Cosmology, 0103 physical sciences, Schwarzschild metric, black hole: Schwarzschild, 010306 general physics, Physics, 010308 nuclear & particles physics, Gravitational wave, Scattering, [PHYS.HTHE]Physics [physics]/High Energy Physics - Theory [hep-th], Regge poles, scattering amplitude, gravitational radiation: scattering, oscillation, angular momentum: complex, wave: electromagnetic, Scattering amplitude, High Energy Physics - Theory (hep-th), General relativity, Quantum electrodynamics, [PHYS.GRQC]Physics [physics]/General Relativity and Quantum Cosmology [gr-qc]
Abstract

We revisit the problem of plane monochromatic gravitational waves impinging upon a Schwarzschild black hole using complex angular momentum techniques. By extending our previous study concerning scalar and electromagnetic waves [A. Folacci and M. Ould El Hadj, Phys.\, Rev.\, D {\bf 99}, 104079, (2019), arXiv:1901.03965], we provide complex angular momentum representations and Regge pole approximations of the helicity-preserving and helicity-reversing scattering amplitudes and of the total differential scattering cross section. We show, in particular, that for high frequencies (i.e., in the short-wavelength regime), a small number of Regge poles permits us to describe numerically with very good agreement the black hole glory and the orbiting oscillations and we then provide a semiclassical approximation that unifies these two phenomena., v2: Close to the published version. arXiv admin note: text overlap with arXiv:1901.03965

Published
2019
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186. Convergence of Fourier-domain templates for inspiraling eccentric compact binaries

Author

Atsushi Nishizawa, Sashwat Tanay, Emanuele Berti, Antoine Klein, Institut d'Astrophysique de Paris (IAP), and Institut national des sciences de l'Univers (INSU - CNRS)-Sorbonne Université (SU)-Centre National de la Recherche Scientifique (CNRS)

Subjects
data analysis method, orbit: velocity, Current (mathematics), media_common.quotation_subject, FOS: Physical sciences, alternative theories of gravity, General Relativity and Quantum Cosmology (gr-qc), 01 natural sciences, General Relativity and Quantum Cosmology, Gravitation, statistical analysis, binary: coalescence, gravitation: weak field, 0103 physical sciences, Convergence (routing), numerical methods, Eccentricity (behavior), numerical calculations, 010303 astronomy & astrophysics, media_common, High Energy Astrophysical Phenomena (astro-ph.HE), Physics, LISA, Series (mathematics), 010308 nuclear & particles physics, Gravitational wave, Mathematical analysis, gravitational radiation, Order (ring theory), black hole: mass, binary: compact, Black hole, error: statistical, black hole: binary, General relativity, orbit: frequency, gravitational radiation: emission, [PHYS.GRQC]Physics [physics]/General Relativity and Quantum Cosmology [gr-qc], Astrophysics::Earth and Planetary Astrophysics, [PHYS.ASTR]Physics [physics]/Astrophysics [astro-ph], Astrophysics - High Energy Astrophysical Phenomena
Abstract

The space-based detector LISA may observe gravitational waves from the early inspiral of stellar-mass black hole binaries, some of which could have significant eccentricity. Current gravitational waveform templates are only valid for small orbital velocities (i.e., in a post-Newtonian expansion) and small initial eccentricity $e_0$ ("post-circular" expansion). We conventionally define $e_0$ as the eccentricity corresponding to an orbital frequency of $5 \text{ mHz}$, and we study the convergence properties of frequency-domain inspiral templates that are accurate up to 2PN and order $e_0^6$ in eccentricity. We compute the so-called "unfaithfulness" between the full template and "reduced" templates obtained by dropping some terms in the phasing series; we investigate the conditions under which systematic errors are negligible with respect to statistical errors, and we study the convergence properties of statistical errors. In general, eccentric waveforms lead to larger statistical errors than circular waveforms due to correlations between the parameters, but the error estimates do not change significantly as long as we include terms of order $e_0^2$ or higher in the phasing., 13 pages, 4 figures

Published
2019
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187. A Multipolar Effective One Body Model for Non-Spinning Black Hole Binaries

Author

Gunnar Riemenschneider, Geraint Pratten, Rossella Gamba, Alessandro Nagar, Institut des Hautes Etudes Scientifiques (IHES), and IHES

Subjects
Physics, 010308 nuclear & particles physics, FOS: Physical sciences, Order (ring theory), alternative theories of gravity, General Relativity and Quantum Cosmology (gr-qc), Function (mathematics), 01 natural sciences, General Relativity and Quantum Cosmology, Gravitation, Black hole, Numerical relativity, Amplitude, General relativity, 0103 physical sciences, Quadrupole, [PHYS.GRQC]Physics [physics]/General Relativity and Quantum Cosmology [gr-qc], Resummation, 010306 general physics, Mathematical physics
Abstract

We introduce \TEOBiResumSM{}, a nonspinning inspiral-merger-ringdown waveform model built within the effective one body (EOB) framework that includes gravitational waveform modes beyond the dominant quadrupole $(\ell,|m|) = (2,2)$. The model incorporates: (i) an improved Pad\'e resummation of the factorized waveform amplitudes $\rho_{\ell m}^{\rm orb}$ entering the EOB-resummed waveform where the 3PN, mass-ratio dependent, terms are hybridized with test-mass limit terms up to 6PN relative order for most of the multipoles up to $\ell=6$ included; (ii) an improved determination of the effective 5PN function $a_6^c(\nu)$ entering the EOB interaction potential done using the most recent, error-controlled, nonspinning numerical relativity (NR) waveforms from the Simulating eXtreme Spacetimes (SXS) collaboration; and (iii) a NR-informed phenomenological description of the multipolar ringdown. Such representation stems from 19 NR waveforms with mass ratios up to $m_1/m_2=18$ as well as test-mass waveform data, although it does not incorporate mode-mixing effects. The NR-completed higher modes through merger and ringdown considered here are: $(\ell,|m|) = \lbrace (2,1), (3,3), (3,2),(3,1),(4,4), (4,3),(4,2), (4,1),(5,5)\rbrace$. For simplicity, the other subdominant modes, up to $\ell=8$, are approximated by the corresponding, purely analytical, factorized and resummed EOB waveform. To attempt an estimate of (some of) the underlying analytic uncertainties of the model, we also contrast the effect of the 6PN-hybrid Pad\'e-resummed $\rho_{\ell m}$'s with the standard $3^{+2}$PN, Taylor-expanded, ones used in previous EOB works. The maximum unfaithfulness $\bar{F}$ against the SXS waveforms including all NR-completed modes up to $\ell=m=5$ is always $\lesssim 2\%$ for binaries with total mass $M$ as $50 M_{\odot} \leq M \lesssim 200 M_{\odot}$., Comment: 24 pages, 18 figures. Improved figures and presentation. Submitted to Phys. Rev. D

Published
2019
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188. How does the photon's spin affect Gravitational Wave measurements?

Author

Loïc Marsot, Centre de Physique Théorique - UMR 7332 (CPT), and Aix Marseille Université (AMU)-Université de Toulon (UTLN)-Centre National de la Recherche Scientifique (CNRS)

Subjects
Physics, Photon, Geodesics in general relativity, 010308 nuclear & particles physics, General relativity, Gravitational wave, spin: effect, gravitational radiation: background, alternative theories of gravity, Polarization (waves), 01 natural sciences, General Relativity and Quantum Cosmology, Gravitational wave background, Quantum electrodynamics, 0103 physical sciences, [PHYS.GRQC]Physics [physics]/General Relativity and Quantum Cosmology [gr-qc], photon: time delay, Spin effect, 010306 general physics, polarization: effect
Abstract

We study the effect of the polarization of light beams on the time delay measured in Gravitational Wave experiments. To this end, we consider the Mathisson-Papapetrou-Dixon equations in a gravitational wave background, with two of the possible spin supplementary conditions: by Frenkel-Pirani, or by Tulczyjew. In the first case, photons follow a null geodesic and thus no spin effect is present. The second case shows a deviation of the photons from the null geodesic, resulting in a tiny effect on the measured time delay of photons depending on their polarization state., Comment: 12 pages; version 2 matches publication with an improved introduction, 14 pages

Published
2019
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189. Stability of scalarized black hole solutions in scalar-Gauss-Bonnet gravity

Author

Hector O. Silva, Jeremy Sakstein, Caio F. B. Macedo, Leonardo Gualtieri, Thomas P. Sotiriou, Emanuele Berti, and SOTIRIOU, THOMAS

Subjects
High Energy Physics - Theory, Black holes, alternative theories of gravity, general relativity, General relativity, Astrophysics::High Energy Astrophysical Phenomena, FOS: Physical sciences, General Relativity and Quantum Cosmology (gr-qc), 01 natural sciences, Instability, General Relativity and Quantum Cosmology, Gravitation, Gauss–Bonnet gravity, 0103 physical sciences, 010306 general physics, High Energy Astrophysical Phenomena, Mathematical physics, High Energy Astrophysical Phenomena (astro-ph.HE), Physics, 010308 nuclear & particles physics, Scalar (physics), Invariant (physics), Black hole, High Energy Physics - Theory (hep-th), Astrophysics - High Energy Astrophysical Phenomena, Scalar field
Abstract

Scalar-tensor theories of gravity where a new scalar degree of freedom couples to the Gauss-Bonnet invariant can exhibit the phenomenon of spontaneous black hole scalarization. These theories admit both the classic black holes predicted by general relativity as well as novel hairy black hole solutions. The stability of the hairy black holes is strongly dependent on the precise form of the scalar-gravity coupling. A radial stability investigation revealed that all scalarized black hole solutions are unstable when the coupling between the scalar field and the Gauss-Bonnet invariant is quadratic in the scalar, whereas stable solutions exist for exponential couplings. Here we elucidate this behavior. We demonstrate that, while the quadratic term controls the onset of the tachyonic instability that gives rise to the black hole hair, the higher-order coupling terms control the nonlinearities that quench that instability, and hence also control the stability of the hairy black hole solutions., Comment: 8 pages, 3 figures. Added citations, updated Fig.2, minor changes to the text. v3: Updated to match published version

Published
2019
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190. Estimating the Parameters of the Hybrid Palatini Gravity Model with the Schwarzschild Precession of S2, S38 and S55 Stars: Case of Bulk Mass Distribution.

Author

Borka, Duško, Borka Jovanović, Vesna, Nikolić, Violeta N., Lazarov, Nenad Đ., and Jovanović, Predrag

Subjects
*GRAVITATIONAL potential, *GENERAL relativity research, *MASS density gradients, *BLACK holes, *STELLAR dynamics, *DARK matter
Abstract

We estimate the parameters of the Hybrid Palatini gravity model with the Schwarzschild precession of S-stars, specifically of the S2, S38 and S55 stars. We also take into account the case of bulk mass distribution near the Galactic Center. We assume that the Schwarzschild orbital precession of mentioned S-stars is the same as in General Relativity (GR) in all studied cases. In 2020, the GRAVITY Collaboration detected the orbital precession of the S2 star around the supermassive black hole (SMBH) at the Galactic Center and showed that it is close to the GR prediction. The astronomical data analysis of S38 and S55 orbits showed that, also in these cases, the orbital precession is close to the GR prediction. Based on this observational fact, we evaluated the parameters of the Hybrid Palatini Gravity model with the Schwarzschild precession of the S2, S38 and S55 stars, and we estimated the range of parameters of the Hybrid Palatini gravity model for which the orbital precession is as in GR for all three stars. We also evaluated the parameters of the Hybrid Palatini Gravity model in the case of different values of bulk mass density distribution of extended matter. We believe that proposed method is a useful tool to evaluate parameters of the gravitational potential at the Galactic Center. [ABSTRACT FROM AUTHOR]

Published
2022
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191. Merging matter and geometry in the same Lagrangian.

Author

Ludwig, Hendrik, Minazzoli, Olivier, and Capozziello, Salvatore

Subjects
*NUCLEAR matter, *LAGRANGIAN functions, *GRAVITY, *GENERAL relativity (Physics), *DUST, *DARK energy
Abstract

We show that a Lagrangian density proportional to − g L m 2 / R reduces to a pressuron theory of gravity that is indistinguishable from General Relativity in the dust limit. The combination of matter and geometry in the same Lagrangian density intrinsically satisfies Mach's Principle — since matter cannot exist without curvature and vice versa — while it may have the correct phenomenology in order to describe actual gravity. [ABSTRACT FROM AUTHOR]

Published
2015
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193. All-sky search for short gravitational-wave bursts in the second Advanced LIGO and Advanced Virgo run

Author

Abbott, B.P., Abbott, R., Abbott, T.D., Abraham, S., Acernese, F., Ackley, K., Adams, C., Adhikari, R.X., Adya, V.B., Affeldt, C., Agathos, M., Agatsuma, K., Aggarwal, N., Aguiar, O.D., Aiello, L., Ain, A., Ajith, P., Allen, G., Allocca, A., Aloy, M.A., Altin, P.A., Amato, A., Anand, S., Ananyeva, A., Anderson, S.B., Anderson, W.G., Angelova, S.V., Antier, S., Appert, S., Arai, K., Araya, M.C., Areeda, J.S., Arène, M., Arnaud, N., Aronson, S.M., Ascenzi, S., Ashton, G., Aston, S.M., Astone, P., Aubin, F., Aufmuth, P., AultONeal, K., Austin, C., Avendano, V., Avila-Alvarez, A., Babak, S., Bacon, P., Badaracco, F., Bader, M.K.M., Bae, S., Baird, J., Baker, P.T., Baldaccini, F., Ballardin, G., Ballmer, S.W., Bals, A., Banagiri, S., Barayoga, J.C., Barbieri, C., Barclay, S.E., Barish, B.C., Barker, D., Barkett, K., Barnum, S., Barone, F., Barr, B., Barsotti, L., Barsuglia, M., Barta, D., Bartlett, J., Bartos, I., Bassiri, R., Basti, A., Bawaj, M., Bayley, J.C., Bazzan, M., Bécsy, B., Bejger, M., Belahcene, I., Bell, A.S., Beniwal, D., Benjamin, M.G., Berger, B.K., Bergmann, G., Bernuzzi, S., Berry, C.P.L., Bersanetti, D., Bertolini, A., Betzwieser, J., Bhandare, R., Bidler, J., Biggs, E., Bilenko, I.A., Bilgili, S.A., Billingsley, G., Birney, R., Birnholtz, O., Biscans, S., Bischi, M., Biscoveanu, S., Bisht, A., Bitossi, M., Bizouard, M.A., Blackburn, J.K., Blackman, J., Blair, C.D., Blair, D.G., Blair, R.M., Bloemen, S., Bobba, F., Bode, N., Boer, M., Boetzel, Y., Bogaert, G., Bondu, F., Bonnand, R., Booker, P., Boom, B.A., Bork, R., Boschi, V., Bose, S., Bossilkov, V., Bosveld, J., Bouffanais, Y., Bozzi, A., Bradaschia, C., Brady, P.R., Bramley, A., Branchesi, M., Brau, J.E., Breschi, M., Briant, T., Briggs, J.H., Brighenti, F., Brillet, A., Brinkmann, M., Brockill, P., Brooks, A.F., Brooks, J., Brown, D.D., Brunett, S., Buikema, A., Bulik, T., Bulten, H.J., Buonanno, A., Buskulic, D., Buy, C., Byer, R.L., Cabero, M., Cadonati, L., Cagnoli, G., Cahillane, C., Calderón Bustillo, J., Callister, T.A., Calloni, E., Camp, J.B., Campbell, W.A., Canepa, M., Cannon, K.C., Cao, H., Cao, J., Carapella, G., Carbognani, F., Caride, S., Carney, M.F., Carullo, G., Casanueva Diaz, J., Casentini, C., Caudill, S., Cavaglià, M., Cavalier, F., Cavalieri, R., Cella, G., Cerdá-Durán, P., Cesarini, E., Chaibi, O., Chakravarti, K., Chamberlin, S.J., Chan, M., Chao, S., Charlton, P., Chase, E.A., Chassande-Mottin, E., Chatterjee, D., Chaturvedi, M., Chatziioannou, K., Cheeseboro, B.D., Chen, H.Y., Chen, X., Chen, Y., Cheng, H.-P., Cheong, C.K., Chia, H.Y., Chiadini, F., Chincarini, A., Chiummo, A., Cho, G., Cho, H.S., Cho, M., Christensen, N., Chu, Q., Chua, S., Chung, K.W., Chung, S., Ciani, G., Cieślar, M., Ciobanu, A.A., Ciolfi, R., Cipriano, F., Cirone, A., Clara, F., Clark, J.A., Clearwater, P., Cleva, F., Coccia, E., Cohadon, P.-F., Cohen, D., Colleoni, M., Collette, C.G., Collins, C., Colpi, M., Cominsky, L.R., Constancio, M., Conti, L., Cooper, S.J., Corban, P., Corbitt, T.R., Cordero-Carrión, I., Corezzi, S., Corley, K.R., Cornish, N., Corre, D., Corsi, A., Cortese, S., Costa, C.A., Cotesta, R., Coughlin, M.W., Coughlin, S.B., Coulon, J.-P., Countryman, S.T., Couvares, P., Covas, P.B., Cowan, E.E., Coward, D.M., Cowart, M.J., Coyne, D.C., Coyne, R., Creighton, J.D.E., Creighton, T.D., Cripe, J., Croquette, M., Crowder, S.G., Cullen, T.J., Cumming, A., Cunningham, L., Cuoco, E., Dal Canton, T., Dálya, G., D’Angelo, B., Danilishin, S.L., D’Antonio, S., Danzmann, K., Dasgupta, A., Da Silva Costa, C.F., Datrier, L.E.H., Dattilo, V., Dave, I., Davier, M., Davis, D., Daw, E.J., DeBra, D., Deenadayalan, M., Degallaix, J., De Laurentis, M., Deléglise, S., Del Pozzo, W., DeMarchi, L.M., Demos, N., Dent, T., De Pietri, R., De Rosa, R., De Rossi, C., DeSalvo, R., de Varona, O., Dhurandhar, S., Díaz, M.C., Dietrich, T., Di Fiore, L., DiFronzo, C., Di Giorgio, C., Di Giovanni, F., Di Giovanni, M., Di Girolamo, T., Di Lieto, A., Ding, B., Di 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Abstract

We present the results of a search for short-duration gravitational-wave transients in the data from the second observing run of Advanced LIGO and Advanced Virgo. We search for gravitational-wave transients with a duration of milliseconds to approximately one second in the 32-4096 Hz frequency band with minimal assumptions about the signal properties, thus targeting a wide variety of sources. We also perform a matched-filter search for gravitational-wave transients from cosmic string cusps for which the waveform is well modeled. The unmodeled search detected gravitational waves from several binary black hole mergers which have been identified by previous analyses. No other significant events have been found by either the unmodeled search or the cosmic string search. We thus present the search sensitivities for a variety of signal waveforms and report upper limits on the source rate density as a function of the characteristic frequency of the signal. These upper limits are a factor of 3 lower than the first observing run, with a 50% detection probability for gravitational-wave emissions with energies of ∼10-9 Mc2 at 153 Hz. For the search dedicated to cosmic string cusps we consider several loop distribution models, and present updated constraints from the same search done in the first observing run. © 2019 American Physical Society.

Published
2019

194. Thermal effects and scalar modes in the cosmological propagation of gravitational waves.

Author

Capozziello, S., Nojiri, S., and Odintsov, S.D.

Abstract

We consider thermal effects in the propagation of gravitational waves on a cosmological background. In particular, we consider scalar field cosmologies and study gravitational modes near cosmological singularities. We point out that the contribution of thermal radiation can heavily affect the dynamics of gravitational waves giving enhancement or dissipation effects both at quantum and classical level. These effects are considered both in General Relativity and in modified theories like F (R) gravity which can be easily reduced to scalar–tensor cosmology. The possible detection and disentanglement of standard and scalar gravitational modes on the stochastic background are also discussed. [ABSTRACT FROM AUTHOR]

Published
2021
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195. A self-dual model for the SU(2) gauge theory.

Author

Zet, G. and Neacsu, C.

Abstract

A model of SU(2) gauge theory in the space time R× S is constructed in terms of local gauge-invariant variables. Ametric tensor g is defined starting with the components of the strength tensor F and of its dual f . It is shown that the components g determine the gauge field equations if some supplementary constraints are imposed. Two families of analytical solutions of the field equations are also obtained. [ABSTRACT FROM AUTHOR]

Published
1999
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196. Dyon field equations in the presence of gravitation.

Author

Rawat, A. and Negi, O.

Abstract

Maxwell's-Dirac field equations of dyons are formulated in the presence of gravitation and the corresponding Lorentz force equation of motion, energy-momentum tensor and Einstein's field equations are derived consistently from an invariant action principle. [ABSTRACT FROM AUTHOR]

Published
1999
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199. Matter imprints in waveform models for neutron star binaries: Tidal and self-spin effects

Author

Tim Dietrich, Alessandro Nagar, Reetika Dudi, M. Pürrer, Chris Van Den Broeck, Sebastiano Bernuzzi, K. W. Tsang, M. Haney, P. Kumar, Francesco Pannarale, Anuradha Samajdar, Sebastian Khan, Gunnar Riemenschneider, Walter Del Pozzo, S. J. Kapadia, Y. Setyawati, Frank Ohme, Charalampos Markakis, Gregorio Carullo, University of Zurich, Institut des Hautes Etudes Scientifiques (IHES), IHES, and Institut des Hautes Etudes Scientifiques ( IHES )

Subjects
neutron star: binary, Physics and Astronomy (miscellaneous), General relativity, 530 Physics, [ PHYS.ASTR ] Physics [physics]/Astrophysics [astro-ph], FOS: Physical sciences, alternative theories of gravity, Binary number, General Relativity and Quantum Cosmology (gr-qc), 10192 Physics Institute, 01 natural sciences, General Relativity and Quantum Cosmology, [ PHYS.GRQC ] Physics [physics]/General Relativity and Quantum Cosmology [gr-qc], Theory of relativity, Binary black hole, numerical methods, 0103 physical sciences, Waveform, 3101 Physics and Astronomy (miscellaneous), numerical calculations, 010306 general physics, orbit, High Energy Astrophysical Phenomena (astro-ph.HE), Physics, 010308 nuclear & particles physics, Gravitational wave, spin: effect, gravitational radiation, Numerical studies of other relativistic binaries, neutron stars, gravitational waves, wave: electromagnetic, Computational physics, Numerical relativity, Neutron star, black hole: binary, gravitation, relativity theory, gravitational radiation: emission, [PHYS.GRQC]Physics [physics]/General Relativity and Quantum Cosmology [gr-qc], Astrophysics - High Energy Astrophysical Phenomena, [PHYS.ASTR]Physics [physics]/Astrophysics [astro-ph], neutron star: coalescence
Abstract

The combined observation of gravitational and electromagnetic waves from the coalescence of two neutron stars marks the beginning of multimessenger astronomy with gravitational waves (GWs). The development of accurate gravitational waveform models is a crucial prerequisite to extract information about the properties of the binary system that generated a detected GW signal. In binary neutron star systems (BNS), tidal effects also need to be incorporated in the modeling for an accurate waveform representation. Building on previous work [Phys. Rev. D 96, 121501 (2017)], we explore the performance of inspiral-merger waveform models that are obtained by adding a numerical relativity (NR) based approximant for the tidal part of the phasing ($\mathrm{NRTidal}$) to existing models for nonprecessing and precessing binary black hole systems, as implemented in the LSC Algorithm Library Suite. The resulting BNS waveforms are compared and contrasted to a set of target waveforms which we obtain by hybridizing NR waveforms (covering the last $\ensuremath{\sim}10$ orbits up to the merger and extending through the postmerger phase) with inspiral waveforms calculated from 30 Hz obtained with a state-of-the-art effective-one-body waveform model. While due to the construction procedure of the target waveforms, there is no error budget available over the full frequency range accessible by advanced GW detectors, the waveform set presents only an approximation of the real signal. We probe that the combination of the self-spin terms and of the $\mathrm{NRTidal}$ description is necessary to obtain minimal mismatches ($\ensuremath{\lesssim}0.01$) and phase differences ($\ensuremath{\lesssim}1\text{ }\text{ }\mathrm{rad}$) with respect to the target waveforms. We also discuss possible improvements and drawbacks of the $\mathrm{NRTidal}$ approximant in its current form.

Published
2019
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200. kiloHertz gravitational waves from binary neutron star remnants: time-domain model and constraints on extreme matter

Author

Albino Perego, M. Agathos, Alessandro Nagar, David Radice, Francesco Zappa, Matteo Breschi, Sebastiano Bernuzzi, Institut des Hautes Etudes Scientifiques (IHES), IHES, Agathos, Michail [0000-0002-9072-1121], and Apollo - University of Cambridge Repository

Subjects
Equation of state, noise, neutron star: binary, gr-qc, Astrophysics::High Energy Astrophysical Phenomena, interferometer, FOS: Physical sciences, alternative theories of gravity, Astrophysics, General Relativity and Quantum Cosmology (gr-qc), Star (graph theory), 01 natural sciences, General Relativity and Quantum Cosmology, star: collapse, binary: coalescence, 0103 physical sciences, numerical methods, black hole, density: high, 010306 general physics, numerical calculations, Astrophysics::Galaxy Astrophysics, equation of state, Physics, High Energy Astrophysical Phenomena (astro-ph.HE), astro-ph.HE, 010308 nuclear & particles physics, Gravitational wave, Shot noise, gravitational radiation, statistical analysis: Bayesian, Radius, gravitational radiation detector, Black hole, Numerical relativity, Neutron star, General relativity, relativity theory, gravitational radiation: emission, [PHYS.GRQC]Physics [physics]/General Relativity and Quantum Cosmology [gr-qc], Astrophysics - High Energy Astrophysical Phenomena
Abstract

International audience; The remnant star of a neutron star merger is an anticipated loud source of kilohertz gravitational waves that conveys unique information on the equation of state of hot matter at extreme densities. Observations of such signals are hampered by the photon shot noise of ground-based interferometers and pose a challenge for gravitational-wave astronomy. We develop an analytical time-domain waveform model for postmerger signals informed by numerical relativity simulations. The model completes effective-one-body waveforms for quasicircular nonspinning binaries in the kilohertz regime. We show that a template-based analysis can detect postmerger signals with a minimal signal-to-noise ratio (SNR) of 8.5, corresponding to GW170817-like events for third-generation interferometers. Using Bayesian model selection and the complete inspiral-merger-postmerger waveform model it is possible to infer whether the merger outcome is a prompt collapse to a black hole or a remnant star. In the latter case, the radius of the maximum mass (most compact) nonrotating neutron star can be determined to kilometer precision. We demonstrate the feasibility of inferring the stiffness of the equation of state at extreme densities using the quasiuniversal relations deduced from numerical-relativity simulations.

Published
2019
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