Testing General Relativity with Present and Future Astrophysical Observations

Berti, Emanuele; Barausse, Enrico; Cardoso, Vitor; Gualtieri, Leonardo; Pani, Paolo; Sperhake, Ulrich; Stein, Leo C.; Wex, Norbert; Yagi, Kent; Baker, Tessa; Burgess, C. P.; Coelho, Flávio S.; Doneva, Daniela; De Felice, Antonio; Ferreira, Pedro G.; Freire, Paulo C. C.; Healy, James; Herdeiro, Carlos; Horbatsch, Michael; Kleihaus, Burkhard; Klein, Antoine; Kokkotas, Kostas; Kunz, Jutta; Laguna, Pablo; Lang, Ryan N.; Li, Tjonnie G. F.; Littenberg, Tyson; Matas, Andrew; Mirshekari, Saeed; Okawa, Hirotada; Radu, Eugen; O'Shaughnessy, Richard; Sathyaprakash, Bangalore S.; Broeck, Chris Van Den; Winther, Hans A.; Witek, Helvi; Aghili, Mir Emad; Alsing, Justin; Bolen, Brett; Bombelli, Luca; Caudill, Sarah; Chen, Liang; Degollado, Juan Carlos; Fujita, Ryuichi; Gao, Caixia; Gerosa, Davide; Kamali, Saeed; Silva, Hector O.; Rosa, João G.; Sadeghian, Laleh; Sampaio, Marco; Sotani, Hajime; Zilhao, Miguel

doi:10.48550/arxiv.1501.07274

Cited by 133 publications

(209 citation statements)

References 761 publications

(1,528 reference statements)

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“…Ref. [60]). Gravastars challenge this paradigm, because they can be as massive and as compact as BHs and, furthermore, they have the same moment of inertia, mass quadrupole moment and even the same (vanishing) tidal Love numbers.…”

Section: Discussionmentioning

confidence: 99%

I-Love-Q relations for gravastars and the approach to the black-hole limit

Pani

2015

Phys. Rev. D

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The multipole moments and the tidal Love numbers of neutron stars and quark stars satisfy certain relations which are almost insensitive to the star's internal structure. A natural question is whether the same relations hold for different compact objects and how they possibly approach the black-hole limit. Here we consider "gravastars", which are hypothetical compact objects sustained by their internal vacuum energy. Such solutions have been proposed as exotic alternatives to the black-hole paradigm because they can be as compact as black holes and exist in any mass range. By constructing slowly-rotating, thin-shell gravastars to quadratic order in the spin, we compute the moment of inertia I, the mass quadrupole moment Q, and the tidal Love number λ in exact form. The I-λ-Q relations of a gravastar are dramatically different from those of an ordinary compact star, but the black-hole limit is continuous, i.e. these quantities approach their Kerr counterparts when the compactness is maximum. Therefore, such relations can be used to discern a gravastar from an ordinary compact star, but not to break the degeneracy with the black-hole case. Based on these results, we conjecture that the full multipolar structure and the tidal deformability of a spinning, ultracompact gravastar are identical to those of a Kerr black hole. The approach to the black-hole limit is nonpolynomial, thus differing from the critical behavior recently found for strongly anisotropic neutron stars. PACS numbers: 04.20.-q, 04.25.-g, 04.70.Bw, 04.30.-w. * paolo.pani@roma1.infn.it 1 At least in the axisymmetric case to second order in the spin [13]and generically to first order in the spin [14].

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Section: Discussionmentioning

confidence: 99%

I-Love-Q relations for gravastars and the approach to the black-hole limit

Pani

2015

Phys. Rev. D

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“…The detection of gravitational waves (GWs) by LIGO (Aasi et al 2015) and Virgo (Acernese et al 2015) has made possible new tests of general relativity (GR) in the strong-field regime (Yunes and Siemens 2013;Berti et al 2015;Yunes et al 2016;Abbott et al 2019Abbott et al , 2020b. Numerous detections of binary coalescences have been made so far (mostly binary black holes) and in the coming years the size of this catalog of detections will continue to grow (Abbott et al 2018).…”

Section: Introductionmentioning

confidence: 99%

Testing general relativity with gravitational-wave catalogs: the insidious nature of waveform systematics

Moore,

Finch,

Buscicchio

et al. 2021

Preprint

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Gravitational-wave observations of binary black holes allow new tests of general relativity to be performed on strong, dynamical gravitational fields. These tests require accurate waveform models of the gravitational-wave signal, otherwise waveform errors can erroneously suggest evidence for new physics. Existing waveforms are generally thought to be accurate enough for current observations, and each of the events observed to date appears to be individually consistent with general relativity. In the near future, with larger gravitational-wave catalogs, it will be possible to perform more stringent tests of gravity by analyzing large numbers of events together. However, there is a danger that waveform errors can accumulate among events: even if the waveform model is accurate enough for each individual event, it can still yield erroneous evidence for new physics when applied to a large catalog. This paper presents a simple linearised analysis, in the style of a Fisher matrix calculation, that reveals the conditions under which the apparent evidence for new physics due to waveform errors grows as the catalog size increases. We estimate that, in the worst-case scenario, evidence for a deviation from general relativity might appear in some tests using a catalog containing as few as 10-30 events above a signal-to-noise ratio of 20. This is close to the size of current catalogs and highlights the need for caution when performing these sorts of experiments.

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“…With the dawn of gravitational-wave astronomy, it is now possible to probe the validity of GR around black holes (BHs) and neutron stars [1,2]. Recently, there has been growing interest in searching for extra degrees of freedom beyond GR and standard model of particle physics in such a strong gravity regime [3,4]. The existence of new degrees of freedom is also motivated by the firm observational evidence of dark matter and dark energy [5][6][7].…”

Section: Introductionmentioning

confidence: 99%

Odd-parity stability of black holes in Einstein-Aether gravity

Tsujikawa,

Zhang,

Zhao

et al. 2021

Preprint

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In Einstein-Aether theory, we study the stability of black holes against odd-parity perturbations on a spherically symmetric and static background. For odd-parity modes, there are two dynamical degrees of freedom arising from the tensor gravitational sector and Aether vector field. We derive general conditions under which neither ghosts nor Laplacian instabilities are present for these dynamical fields. We apply these results to concrete black hole solutions known in the literature and show that some of those solutions can be excluded by the violation of stability conditions. The exact Schwarzschild solution present for c13 = c14 = 0, where ci's are the four coupling constants of the theory with cij = ci + cj , is prone to Laplacian instabilities along the angular direction throughout the horizon exterior. However, we find that the odd-parity instability is absent for black hole solutions with c13 = c4 = 0 and c1 ≥ 0.

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Testing General Relativity with Present and Future Astrophysical Observations

Cited by 133 publications

References 761 publications

I-Love-Q relations for gravastars and the approach to the black-hole limit

I-Love-Q relations for gravastars and the approach to the black-hole limit

Testing general relativity with gravitational-wave catalogs: the insidious nature of waveform systematics

Odd-parity stability of black holes in Einstein-Aether gravity

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