Perturbations of Spinning Black Holes beyond General Relativity: Modified Teukolsky Equation

Li, Dongjun; Wagle, P. M.; Chen, Yanbei; Yunes, Nicolás

doi:10.1103/physrevx.13.021029

Cited by 36 publications

(6 citation statements)

References 161 publications

Supporting

Mentioning

Contrasting

Order By: Relevance

“…However, we strongly expect that the higher-order PN corrections will be an interesting addition to such an analysis, which we hope to communicate in our upcoming studies. Another direction to explore these scenarios is the black hole perturbation [113,114] that can more concretely improvise the PN results and can constrain the deviation parameters with their possible detectability. If LISA might impose interesting limits on non-GR deviations/deformations, it is an intriguing topic that could be addressed with the aid of the Johannsen framework.…”

Section: Discussionmentioning

confidence: 99%

Prospects of detecting deviations to Kerr geometry with radiation reaction effects in EMRIs

Chowdhuri,

Bhattacharyya,

Kumar

2024

J. Cosmol. Astropart. Phys.

View full text Add to dashboard Cite

Direct detection of gravitational waves and binary black hole mergers have proven to be remarkable investigations of general relativity. In order to have a definitive answer as to whether the black hole spacetime under test is the Kerr or non-Kerr, one requires accurate mapping of the metric. Since EMRIs are perfect candidates for space-based detectors, Laser Interferometer Space Antenna (LISA) observations will serve a crucial purpose in mapping the spacetime metric. In this article, we consider such a study with the Johannsen spacetime that captures the deviations from the Kerr black hole and further discuss their detection prospects. We analytically derive the leading order post-Newtonian corrections in the average loss of energy and angular momentum fluxes generated by a stellar-mass object exhibiting eccentric equatorial motion in the Johannsen background. We further study the orbital evolution of the inspiralling object within the adiabatic approximation. We lastly provide the possible detectability of deviations from the Kerr black hole by estimating gravitational wave dephasing and highlight the crucial role of LISA observations.

show abstract

Section: Discussionmentioning

confidence: 99%

Prospects of detecting deviations to Kerr geometry with radiation reaction effects in EMRIs

Chowdhuri,

Bhattacharyya,

Kumar

2024

J. Cosmol. Astropart. Phys.

View full text Add to dashboard Cite

show abstract

“…In both cases, it would be valuable to connect more closely and in more generality to the large literature on solutions to the wave equation on a rotating black hole background [89,96,97,116]. This could include using higher-spin fields and making contact to the Teukolsky equation [117], as opposed to the scalar wave equations used here, considering other modifications to the wave equations, as for example in modified theories of gravity or black holes [68,[118][119][120][121][122][123][124][125][126][127], the introduction of sources [128,129], investigating how to describe caustics as well as the propagator and scattering on the black hole background more generally [130][131][132][133][134]. To do so, it will be important to understand the matched asymptotic expansion that embeds the plane wave into the full spacetime, and the respective interplay between the 'far-zone' outer spacetime and the 'near-zone' plane wave.…”

Section: Discussionmentioning

confidence: 99%

Quasinormal modes from Penrose limits

Fransen

2023

Class. Quantum Grav.

View full text Add to dashboard Cite

We use Penrose limits to approximate quasinormal modes with large real frequencies. The Penrose limit associates a plane wave to a region of spacetime near a null geodesic. This plane wave can be argued to geometrically realize the geometrical optics approximation. Therefore, when applied to the bound null orbits around black holes, the Penrose limit can be used to study quasinormal modes. For instance, this Penrose limit point of view makes manifest the symmetry that emerges in the geometrical optics approximation of quasinormal modes in terms of isometries of the resulting plane wave spacetime. We apply the procedure to warped AdS3, Schwarzschild black holes and Kerr black holes. In the former we show explicitly how the symmetry algebra contracts to that of the limiting plane wave while in the latter we ﬁnd the expected agreement with numerically computed quasinormal modes for large (real) frequencies.

show abstract

“…We note in passing that describing the registered gravitational events as waves is misleading: normal modulation of the gravitational potential, registered by LIGO and Virgo interferometers, and caused by rotating (in the merger case, inspiral) objects, is wrongly interpreted as a gravitational wave understood as a carrier of gravity [87]. Furthermore, it has been suggested that outside the GR, merging BHs may differ from their GR counterparts [88].…”

Section: Bb Mergersmentioning

confidence: 91%

The Imaginary Universe

Łukaszyk

2024

Preprint

View full text Add to dashboard Cite

Maxwell's equations in vacuum provide the negative speed of light -c, which leads to imaginary Planck units. However, the second, negative fine-structure constant $\alpha_2^{-1} \approx -140.178$, present in the Fresnel coefficients for the normal incidence of electromagnetic radiation on monolayer graphene, establishes the different, negative speed of light in vacuum $c_2 \approx -3.06 \times 10^8~\text{[m/s]}$, which introduces imaginary Planck units different in magnitude from those parametrized with $c$. Furthermore, algebraic relations between the fine-structure constant hint that the fine-structure constant does not vary over time. It follows that electric charges are the same in real and imaginary dimensions. We model neutron stars and white dwarfs, emitting perfect black-body radiation, as \textit{objects} having energy exceeding their mass-energy equivalence ratios. We define complex energies in terms of real and imaginary natural units. Their imaginary parts, inaccessible for direct observation, store the excess of these energies. It is conjectured that the maximum atomic number $Z=238$. A black-body \textit{object} is in the equilibrium of complex energies if its radius $R_\text{eq} \approx 1.3833~R_{\text{BH}}$, which is close to the photon sphere radius $R_{\text{ps}}=1.5~R_{\text{BH}}$, and marginally greater than a locally negative energy density bound of $4/3~R_{\text{BH}}$. The complex force between real masses and imaginary charges leads to the black-body object's surface gravity and generalized Hawking radiation temperature, which includes its charge. Furthermore, this force agrees with the physical parameters of the hydrogen atom. The proposed model takes into account the value(s) of the fine-structure constant(s), which is/are otherwise neglected in general relativity, and explains the registered (GWOSC) high masses of neutron stars' mergers and the associated fast radio bursts (CHIME) without resorting to any hypothetical types of exotic stellar \textit{objects}.

show abstract

Perturbations of Spinning Black Holes beyond General Relativity: Modified Teukolsky Equation

Cited by 36 publications

References 161 publications

Prospects of detecting deviations to Kerr geometry with radiation reaction effects in EMRIs

Prospects of detecting deviations to Kerr geometry with radiation reaction effects in EMRIs

Quasinormal modes from Penrose limits

The Imaginary Universe

Contact Info

Product

Resources

About