We have studied the null geodesics in the background of the Kerr–Newman black hole veiled by a plasma medium using the Hamilton–Jacobi method. The influence of black hole's charge and plasma parameters on the effective potential and the generic photon orbits has been investigated. Furthermore, our discussion embodies the effects of black …

Duncan was born in January 14, 1955 Duncan has 6 phone numbers Duncan has 4 relatives Duncan has 8 past addresses Duncan has 10 associates by phone number Duncan has 38 associates by address Duncan is married Duncan's home type is Single Family Dwelling Unit The property where Duncan lives was built in 1976 Duncan has …

Resides in Milwaukee, WI. Lived In Lexington KY, Grosse Pointe MI, Earleton FL, Melrose FL. Related To Joseph Kerr, Timothy Kerr, Christopher Kerr, Margaret Kerr, Melissa Kerr. Also known as Susan K Duncan, S L Kerr. Includes Address (11) …

The FWT Hamiltonian for a Dirac particle in the Kerr geometry in a slowly rotating, weak-field limit is given in Konno and Kasai (1998); Konno (1998). For non-relativistic limit and rotating central object with uniform mass density, the Hamiltonian for the Dirac fermion in Kerr gravitational field becomes: H = m c 2 + p 2 2 m + m ϕ − ω p →.

Gravitational Faraday Rotation (GFR) is a frame-dragging effect induced by rotating massive objects, which is one of the important, yet studied characteristics of lensed gravitational waves (GWs). In this work, we calculate the GFR angle $χ_g$ of GWs in the weak deflection limit, assuming it is lensed by a Kerr black hole (BH). We find that the …

It was shown recently that the static tidal response coefficients, called Love numbers, vanish identically for Kerr black holes in four dimensions. In this work, we confirm this result and extend it to the case of spin-0 and spin-1 perturbations. We compute the static response of Kerr black holes to scalar, electromagnetic, and gravitational fields at all …

Alison Duncan Kerr has been continuously employed by the University of St. Andrews since 2017. In 2018, she obtained a 3-year research fellowship in order to establish the St Andrews Institute of Gender Studies (StAIGS) and a new Gender Studies MLitt program. It appears that in many ways she went above and beyond what was expected …

In the bag model, we keep untouched the external Kerr–Newman gravitational field, and create inside the bag the vacuum state designed for action of quantum theory. The bag model formed by the domain wall solution interpolates between the external Kerr–Newman solution and the internal flat core. As the Higgs field gives a …

We study the strong gravitational lensing on the equatorial plane of a quasi-Kerr compact object with arbitrary quadrupole moments which can be used to model the super-massive central object of the galaxy. We find that, when the quadrupolar correction parameter ξ takes the positive (negative) value, the photon-sphere radius r ps, …

gravitational field of a third stellar-mass object [17–20], the migration force from an accretion disk and/or the interaction between the stellar-mass black hole and a possible dark-matter cloud [21–28]. From the perspective of testing General Rela-tivity, it is interesting to test the Kerr metric as a key predic-

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@article{osti_21432383, title = {Gravitational radiation from a spinning compact object around a supermassive Kerr black hole in circular orbit}, author = {Wenbiao, Han}, abstractNote = {The gravitational waves and energy radiation from a spinning compact object with stellar mass in a circular orbit in the equatorial plane of a …

A bstract. We revisit the spectrum of linear axisymmetric gravitational perturbations of the (near-)extreme Kerr black hole. Our aim is to characterise those perturbations that are responsible for the deviations away from extremality, and to contrast them with the linearized perturbations treated in the Newman-Penrose formalism.

the exterior gravitational eld of a spherically symmetric mass. The Kerr solution is only unique if the multipole moments of its mass and its angular momentum take on prescribed values. Its metric can be interpreted as the exterior gravitational eld of a suitably rotat-ing mass distribution. Both solutions describe objects exhibiting an

In our study, we use geometric units c = G = M = 1. The Kerr metric is an axially symmetric, stationary vacuum solution to the Einstein field equations, which describes uncharged rotating compact ...

These quantities are of interest in gravitational-wave astronomy, to test the so-called "no-hair theorem" of general relativity, and in the context of the gauge-gravity duality. Here you can find data for: the QNM spectrum of Schwarzschild (anti-de Sitter) and Kerr black holes. the excitation factors of Kerr quasinormal modes.

In this review, motivated primarily by small-mass-ratio binaries but not limited to them, we provide an overview of essential methods in (i) black hole perturbation …

the ratio of the gravitational radius of the black hole, r g ≡ GM/c 2, to the (reduced) Compton wav elength of the field, λ c ≡ ~ / ( µc ), where µ is the mass of the …

As such, even if black holes are Kerr, the underlying theory can, in principle, be probed through gravitational distortions. In this paper, we study linear perturbations of a Kerr black hole in f (R) gravity using the Newman-Penrose formalism. We show that, as in general relativity, the equations governing the perturbed metric, which depend on ...

We compute the static response of Kerr black holes to scalar, electromagnetic, and gravitational fields at all orders in black hole spin. We use the unambiguous and gauge-invariant definition of Love numbers and their spin-0 and spin-1 analogs as Wilson coefficients of the point particle effective field theory.

In a 912-page paper posted online on May 30, Szeftel, Elena Giorgi of Columbia University and Sergiu Klainerman of Princeton University have proved that slowly rotating Kerr black holes are indeed stable. The work is the product of a multiyear effort. The entire proof — consisting of the new work, an 800-page paper by Klainerman and Szeftel …

The different calculations carried out in the past to understand the propagation of a light ray in a rotating gravitational field (viz Kerr field) are examined. For a plane-polarized light ray, it ...

Our analysis includes their effects on the line element, their contributions to Iyer-Wald charges around the NHEK geometry, and how to reconstitute them as …

the ratio of the gravitational radius of the black hole, r g ≡ GM/c 2, to the (reduced) Compton wav elength of the field, λ c ≡ ~ / ( µc ), where µ is the mass of the field. This defines ...

Gravitational perturbations from NHEK to Kerr Alejandra Castro, Victor Godet, Joan Simón, Wei Song, Boyang Yu We revisit the spectrum of linear …

observer inclinations in a Kerr gravitational lens. Therefore the purpose of this paper is two-fold. First, to extend the study of relativistic images for the case when the gravitational deflector is a rotating Kerr black hole. Secondly, since the trajectory of a photon will not always will be confined to a plane, we shall also be con-

Author note: The authors thank Alison Duncan Kerr, Juli e Huang, and the members of th e Social Cognitive Science Lab for helpful comm ents on an earlier version of this article.

We study the strong gravitational lensing due to the Kerr black holes with angular momentum and the Kerr-Newman black holes with additional charge Q. We rst derive …

Abstract. A class of new inhomogeneous equations governing gravitational perturbations of the Kerr geometry is presented. It is shown that, contrary to the case of …

The gravitational lensing of relativistic neutral massive particles caused by a Kerr-Newman black hole is investigated systematically in the weak-field limit. Based on the Kerr-Newman metric in Boyer-Lindquist coordinates, we first derive the analytical form of the equatorial gravitational deflection angle of a massive particle in the third post …