Numerical black hole initial data and shadows in dynamical Chern–Simons gravity

Okounkova, Maria; Scheel, Mark A.; Teukolsky, Saul A.

doi:10.1088/1361-6382/aafcdf

Cited by 22 publications

(27 citation statements)

References 52 publications

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“…Future work in this program thus involves adding initial orbital angular momentum to the system and producing beyond-GR gravitational waveforms for inspiraling systems. We have previously evolved the leading order dCS scalar field for an inspiraling BBH background [11], and can use our (fully-general) methods given in [12] and [13] to produce initial data for and evolve an inspiraling BBH system.…”

Section: Discussionmentioning

confidence: 99%

“…(11) computed from ∆ϑ instead of ϑ (1) , and C (1) ab [∆ϑ] similarly refers to the C-tensor in Eq. (12) computed with ∆ϑ instead of ϑ (1) .…”

Section: Scaled Variablesmentioning

confidence: 99%

“…The scalar field initial data are given by a superposition of slow-rotation solutions [11,30,31]. The constraint-satisfying initial data for ∆g ab are generated using the methods outlined in [12]. For head-on collisions, we start with a separation of 25 M , assuming that the contributions to the gravitational radiation and energy flux from times t 25 M are negligible.…”

Section: Initial Datamentioning

confidence: 99%

“…When solving for perturbed initial data (cf. [12]), we similarly have the freedom to choose ∂ t ∆α and ∂ t ∆β i , the time derivatives of the perturbed lapse and shift. An easy choice, for example, is to work in a perturbed harmonic gauge,…”

Section: Appendix B: Choosing a Perturbed Gaugementioning

confidence: 99%

“…All of the perturbed quantities ∆g ij , ∆K ij , ∆(D k K ij ), and ∆R ij are given in terms of the perturbation to the spatial metric, ∆γ ij = ∆g ij , its spatial derivative ∂ k ∆γ ij = ∂ k ∆g ab , and its time derivative, ∂ t ∆γ ij = ∂ t ∆g ij in [12]. Note that since we use a first-order scheme, we have access to ∆g ab , ∂ c ∆g ab throughout the evolution (cf.…”

Section: Appendix C: Computing Perturbed Gravitational Radiationmentioning

confidence: 99%

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Numerical binary black hole collisions in dynamical Chern-Simons gravity

et al. 2019

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We produce the first numerical relativity binary black hole gravitational waveforms in a highercurvature theory beyond general relativity. In particular, we study head-on collisions of binary black holes in order-reduced dynamical Chern-Simons gravity. This is a precursor to producing beyond-general-relativity waveforms for inspiraling binary black hole systems that are useful for gravitational wave detection. Head-on collisions are interesting in their own right, however, as they cleanly probe the quasi-normal mode spectrum of the final black hole. We thus compute the leading-order dynamical Chern-Simons modifications to the complex frequencies of the post-merger gravitational radiation. We consider equal-mass systems, with equal spins oriented along the axis of collision, resulting in remnant black holes with spin. We find modifications to the complex frequencies of the quasi-normal mode spectrum that behave as a power law with the spin of the remnant, and that are not degenerate with the frequencies associated with a Kerr black hole of any mass and spin. We discuss these results in the context of testing general relativity with gravitational wave observations.

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Section: Discussionmentioning

confidence: 99%

“…(11) computed from ∆ϑ instead of ϑ (1) , and C (1) ab [∆ϑ] similarly refers to the C-tensor in Eq. (12) computed with ∆ϑ instead of ϑ (1) .…”

Section: Scaled Variablesmentioning

confidence: 99%

Section: Initial Datamentioning

confidence: 99%

Section: Appendix B: Choosing a Perturbed Gaugementioning

confidence: 99%

Section: Appendix C: Computing Perturbed Gravitational Radiationmentioning

confidence: 99%

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Numerical binary black hole collisions in dynamical Chern-Simons gravity

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A Beginner’s Guide to Black Hole Imaging and Associated Tests of General Relativity

Lupsasca,

Mayerson,

Ripperda

et al. 2024

Recent Progress on Gravity Tests

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Photon ring test of the Kerr hypothesis: Variation in the ring shape

Paugnat

Lupsasca

Vincent

et al. 2022

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Context. The Event Horizon Telescope (EHT) collaboration recently released horizon-scale images of the supermassive black hole M87*. These images are consistently described by an optically thin, lensed accretion flow in the Kerr spacetime. General relativity (GR) predicts that higher-resolution images of such a flow would present thin, ring-shaped features produced by photons on extremely bent orbits. Recent theoretical work suggests that these "photon rings" produce clear interferometric signatures that depend very little on the astrophysical configuration and whose observation could therefore provide a stringent consistency test of the Kerr hypothesis. Aims. We wish to understand how the photon rings of a Kerr black hole vary with its surrounding emission. Gralla, Lupsasca, and Marrone (GLM) found that the shape of high-order photon rings follows a specific functional form that is insensitive to the details of the astrophysical source, and proposed a method for measuring this GR-predicted shape via space-based interferometry. We wish to assess the robustness of this prediction by checking it for a variety of astrophysical profiles, black hole spins, and observer inclinations. Methods. We use the ray tracing code Gyoto to simulate images of thin equatorial disks accreting onto a Kerr black hole. We extract the shape of the resulting photon rings from their interferometric signatures using a refinement of the method developed by GLM. We repeat this analysis for hundreds of models with different emission profiles, black hole spins, and observer inclinations. Results. We identify the width of the photon ring and its angular variation as a main obstacle to the method's success. We qualitatively describe how this width varies with the emission profile, black hole spin, and observer inclination. At low inclinations, our improved method is robust enough to confirm the shape prediction for a variety of emission profiles; however, the choice of baseline is critical to the method's success. At high inclinations, we encounter qualitatively new effects that are caused by the ring's non-uniform width and require further refinements to the method. We also explore how the photon ring shape could constrain black hole spin and inclination.

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Numerical black hole initial data and shadows in dynamical Chern–Simons gravity

Cited by 22 publications

References 52 publications

Numerical binary black hole collisions in dynamical Chern-Simons gravity

Numerical binary black hole collisions in dynamical Chern-Simons gravity

A Beginner’s Guide to Black Hole Imaging and Associated Tests of General Relativity

Photon ring test of the Kerr hypothesis: Variation in the ring shape

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