Kerr-Taub-NUT spacetime with Maxwell and dilaton fields

Aliev, Alikram N.; Cebeci, Hakan; Dereli, Tekin

doi:10.1103/physrevd.77.124022

Cited by 42 publications

(44 citation statements)

References 32 publications

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“…However, for the motion in equatorial plane (θ = π/2) the equation of motion maybe separable in spacetimes having symmetries and one may proceed the calculations for the equatorial motion (see [63]). Inserting (26) to (25) and after making calculations in equatorial plane (θ = π/2) one can easily find the equation for the radial part of motion which corresponds to the radial component of covariant 4-momentum of the charged particle (p r = ∂S r /∂r). Radial contravariant component of the momentum can be obtained multiplying the metric (1) with covariant momentum.…”

Section: Charged Particle Motion Around Magnetized Compact Objectmentioning

confidence: 99%

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Charged particle motion around a quasi-Kerr compact object immersed in an external magnetic field

et al. 2019

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We explore the electromagnetic fields around a quasi-Kerr compact object assuming it is immersed in an external asymptotically uniform magnetic field. Using the Wald method, components of the electromagnetic field in orthonormal basis have been obtained. We explore the charged particle motion around deformed Kerr compact objects in the presence of external asymptotically uniform magnetic fields. Using the Hamilton-Jacobi equation, we obtain the effective potential expression for the charged particle surrounding a quasi-Kerr compact object immersed in an external magnetic field. It is also derived the dependence of innermost stable circular orbits (ISCOs) from the magnetic and deformation parameters for charged particles motion around a rotating quasi-Kerr compact object. Comparison with ISCO radius measurements has provided the constraint to the deformation parameter as −0.012. The center of mass (CM) energy of the colliding particles in several physically interesting cases has been studied.

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Section: Charged Particle Motion Around Magnetized Compact Objectmentioning

confidence: 99%

“…The properties of the black holes with brane charge have been studied in [18][19][20][21][22]. Other extension of the Kerr solution is the solution with gravitomagnetic charge [2,[23][24][25][26][27][28]. Various works are dedicated to test the axial symmetric metrics with the deformation parameters [29][30][31][32][33][34][35][36][37].…”

Section: Introductionmentioning

confidence: 99%

Charged particle motion around a quasi-Kerr compact object immersed in an external magnetic field

et al. 2019

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“…KerrTaub-NUT metrics, meanwhile, are parametrized by mass, spin, and l, with l ≠ 0, and are thought to be unphysical [84]. The vacuum BBH case considered in this study, meanwhile, sets e ¼ 0 and g ¼ 0, since there are no electric or magnetic charges at the start of the simulation, and no sourcing of them during the simulation.…”

Section: Appendix: Kerr-nut Parametersmentioning

confidence: 99%

On choosing the start time of binary black hole ringdowns

et al. 2018

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The final stage of a binary black hole merger is ringdown, in which the system is described by a Kerr black hole with quasinormal mode perturbations. It is far from straightforward to identify the time at which the ringdown begins. Yet determining this time is important for precision tests of the general theory of relativity that compare an observed signal with quasinormal mode descriptions of the ringdown, such as tests of the no-hair theorem. We present an algorithmic method to analyze the choice of ringdown start time in the observed waveform. This method is based on determining how close the strong field is to a Kerr black hole (Kerrness). Using numerical relativity simulations, we characterize the Kerrness of the strong-field region close to the black hole using a set of local, gauge-invariant geometric and algebraic conditions that measure local isometry to Kerr. We produce a map that associates each time in the gravitational waveform with a value of each of these Kerrness measures; this map is produced by following outgoing null characteristics from the strong and near-field regions to the wave zone. We perform this analysis on a numerical relativity simulation with parameters consistent with GW150914-the first gravitational-wave detection. We find that the choice of ringdown start time of 3 ms after merger used in the GW150914 study [B. P. Abbott et al. (Virgo Collaboration and LIGO Scientific Collaboration), Phys. Rev. Lett. 116, 221101 (2016).] to test general relativity corresponds to a high dimensionless perturbation amplitude of ∼7.5 × 10 −3 in the strong-field region. This suggests that in higher signal-to-noise detections, one would need to start analyzing the signal at a later time for studies that depend on the validity of black hole perturbation theory.

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“…Nouri-Zonoz 2004; Kagramanova et al 2008;Morozova and Ahmedov 2009, where solutions for electromagnetic waves and interferometry in spacetime with NUT parameter have been studied). Kerr-Taub-NUT spacetime with Maxwell and dilation fields is recently investigated by Aliev et al (2008). In our preceding papers (Morozova et al 2008;Abdujabbarov et al 2008) we have studied the plasma magnetosphere around a rotating, magnetized neutron star and charged particle motion around compact objects immersed in external magnetic field in the presence of the NUT parameter.…”

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confidence: 99%