Analytical and numerical treatment of perturbed black holes in horizon-penetrating coordinates

Bhattacharyya, Maitraya K.; Hilditch, David; Nayak, K. Rajesh; Rüter, Hannes R.; Brügmann, Bernd

doi:10.1103/physrevd.102.024039

Cited by 8 publications

(10 citation statements)

References 72 publications

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“…The event horizon of the corresponding black hole is at and the (dimensionless) ADM mass is 57 . As mentioned earlier, the remnant black hole decreases its energy content, inducing a change in the metric mass-function from the initial, dimensionless Schwarzschild value 58 , 59 : Assuming the mode functions to be regular and slowly varying in close to horizon 52 , 53 , 60 , and expanding both sides of Eq. ( 32 ) for the component, we get (See supplementary material 33 for details): where and denotes derivative with respect to V .…”

Section: Backreaction Of the Emitted Gravitational Wavesmentioning

confidence: 99%

The dominating mode of two competing massive modes of quadratic gravity

Chowdhury

Xavier

Shankaranarayanan

2023

Sci Rep

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Over the last two decades, motivations for modified gravity have emerged from both theoretical and observational levels. f(R) and Chern-Simons gravity have received more attention as they are the simplest generalization. However, f(R) and Chern-Simons gravity contain only an additional scalar (spin-0) degree of freedom and, as a result, do not include other modes of modified theories of gravity. In contrast, quadratic gravity (also referred to as Stelle gravity) is the most general second-order modification to 4-D general relativity and contains a massive spin-2 mode that is not present in f(R) and Chern-Simons gravity. Using two different physical settings—the gravitational wave energy-flux measured by the detectors and the backreaction of the emitted gravitational radiation on the spacetime of the remnant black hole—we demonstrate that massive spin-2 mode carries more energy than the spin-0 mode. Our analysis shows that the effects are pronounced for intermediate-mass black holes, which are prime targets for LISA.

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Section: Backreaction Of the Emitted Gravitational Wavesmentioning

confidence: 99%

The dominating mode of two competing massive modes of quadratic gravity

Chowdhury

Xavier

Shankaranarayanan

2023

Sci Rep

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“…It is the general Heun polynomial solution for the scalar particle containing confluent Heun function (HeunC).First part of this solution is for in going, while second part is for outgoing particle. HeunC can be expanded for N order by using two polynomial conditions [10,21,22] and these condition gives specific energy for given mass of stable orbit. Two polynomial conditions are…”

Section: Quasi Normal Modesmentioning

confidence: 99%

“…The focus of my work revolves around addressing the unresolved issues mentioned in the previous paragraph. In the first section, I calculate the potential energy using the tortoise coordinate system [1,2,3,4,5,6] for the Klein-Gordon equation in the Schwarzschild black hole [6,7,8,9,10,11]. Furthermore, I present the minimum distance from the event horizon required for a stable orbit.…”

Section: Introductionmentioning

confidence: 99%

“…The second section focuses on determining the energy of quasi-normal modes [9,12,13,14,15,16,17,18,19] for different values of the polynomial order of the HeunC function. Additionally, I establish the relationship between complex energy and order by employing two polynomial conditions [10,21,22] on the HeunC function. Based on these findings, I obtain the relation between the real and imaginary values of energy.…”

Section: Introductionmentioning

confidence: 99%

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Stable orbit of Massive Klein Gordon Field near Schawarzschild black hole and its Quasi-Normal modes

Sharma¹

2023

Preprint

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The findings of bound states of the massive Klein-Gordon field near the Schwarzschild black hole have provided certain conditions for a stable orbit. Unlike classical methods, I have obtained a specific relation between the mass of the scalar particle and the distance from the black hole. Furthermore, by applying a polynomial condition to the Heun function, more accurate predictions of quasi-normal modes have been made. Based on this, the time of a stable orbit and its relationship with mass, polynomial order, and distance from the Schwarzschild black hole have been calculated.

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“…An additional motivation to use Kerr-Schild coordinates lies in the fact that the exact analytical solution of the Einstein's field equation for a moving rotating black hole in standard coordinates is too lengthy to be applied conveniently, although the metrics of static or stationary black holes in Boyer-Linquist coordinates are elegant and have been adopted by lots of work (See, for instance, Refs. [47][48][49][50].…”

Section: Introductionmentioning

confidence: 99%

Kerr-Schild Form of the Exact Metric for a Constantly Moving Kerr Black Hole and Null Gravitational Deflection

Li,

Feng,

Zhou

et al. 2021

Preprint

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The exact metric of a moving Kerr black hole with an arbitrary constant velocity is derived in Kerr-Schild coordinates. We then calculate the null equatorial gravitational deflection caused by a radially moving Kerr source up to the second post-Minkowskian order, acting as an application of the weak field limit of the metric. The bending angle of light is found to be consistent with the result given in the previous works.

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Analytical and numerical treatment of perturbed black holes in horizon-penetrating coordinates

Cited by 8 publications

References 72 publications

The dominating mode of two competing massive modes of quadratic gravity

The dominating mode of two competing massive modes of quadratic gravity

Stable orbit of Massive Klein Gordon Field near Schawarzschild black hole and its Quasi-Normal modes

Kerr-Schild Form of the Exact Metric for a Constantly Moving Kerr Black Hole and Null Gravitational Deflection

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