Does a black hole rotate in Chern-Simons modified gravity?

Konno, Kohkichi; Matsuyama, Toyoki; Tanda, Satoshi

doi:10.1103/physrevd.76.024009

Cited by 46 publications

(69 citation statements)

References 20 publications

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“…The first solutions were found by Alexander and Yunes [8,9], using a far-field approximation (where the field point distance is considered to be much larger than the black hole mass). The second rotating black hole solution was found by Konno et al [10], using a small slow-rotation approximation, where the spin angular momentum is assumed to be much smaller than the black hole mass. However, it is interesting to note that recently, using the dynamical formulation of CS modified gravity, spinning black hole solutions in the slow-rotation approximation have been obtained [11,12].…”

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confidence: 99%

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Thin accretion disk signatures in dynamical Chern–Simons-modified gravity

Harkó

Kovács

Lobo

2010

Class. Quantum Grav.

104

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A promising extension of general relativity is Chern-Simons (CS) modified gravity, in which the Einstein-Hilbert action is modified by adding a parity-violating CS term, which couples to gravity via a scalar field. In this work, we consider the interesting, yet relatively unexplored, dynamical formulation of CS modified gravity, where the CS coupling field is treated as a dynamical field, endowed with its own stress-energy tensor and evolution equation. We consider the possibility of observationally testing dynamical CS modified gravity by using the accretion disk properties around slowly-rotating black holes. The energy flux, temperature distribution, the emission spectrum as well as the energy conversion efficiency are obtained, and compared to the standard general relativistic Kerr solution. It is shown that the Kerr black hole provide a more efficient engine for the transformation of the energy of the accreting mass into radiation than their slowly-rotating counterparts in CS modified gravity. Specific signatures appear in the electromagnetic spectrum, thus leading to the possibility of directly testing CS modified gravity by using astrophysical observations of the emission spectra from accretion disks.

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confidence: 99%

“…date, has considered the nondynamical formulation [7][8][9][10], whereas the dynamical formulation remains mostly unexplored territory.…”

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confidence: 99%

Thin accretion disk signatures in dynamical Chern–Simons-modified gravity

Harkó

Kovács

Lobo

2010

Class. Quantum Grav.

104

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“…Konno, Matsuyama, Asano and Tanda [33] (hereafter KMAT) studied a solution for a slowly rotating black hole in CS modified gravity derived previously by Konno, Matsuyama and Tanda [34] (hereafter KMT). The KMT slow rotating solution corresponds to a (special) spatial coupling field.…”

Section: Introductionmentioning

confidence: 99%

“…In this paper, we shall consider the KMT solution [33,34] to study the effects of CS modified gravity on the phase shift in neutron interferometry using, in addition, the equations of optical-mechanical analogy for rotating sources [36]. The final formula for phase shift shows a combination of different effects.…”

Section: Introductionmentioning

confidence: 99%

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Quantum phase shift in Chern-Simons modified gravity

Nandi

Kizirgulov²,

Mikolaychuk³

et al. 2009

Phys. Rev. D

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Using a unified approach of optical-mechanical analogy in a semiclassical formula, we evaluate the effect of Chern-Simons modified gravity on the quantum phase shift of de Broglie waves in neutron interferometry. The phase shift calculated here reveals, in a single equation, a combination of effects coming from Newtonian gravity, inertial forces, Schwarzschild and Chern-Simons modified gravity. However the last two effects, though new, turn out to be too tiny to be observed, and hence only of academic interest at present. The approximations, wherever used, as well as the drawbacks of the non-dynamical approach are clearly indicated. PACS numbers(s): 95.85. Ry, 12.15.Ff, 04.50.+h

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Leading higher-derivative corrections to Kerr geometry

Cano

Ruipérez

2019

J. High Energ. Phys.

103

108

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We compute the most general leading-order correction to Kerr solution when the Einstein-Hilbert action is supplemented with higher-derivative terms, including the possibility of dynamical couplings controlled by scalars. The model we present depends on five parameters and it contains, as particular cases, Einstein-dilaton-Gauss-Bonnet gravity, dynamical Chern-Simons gravity and the effective action coming from Heterotic Superstring theory. By solving the corrected field equations, we find the modified Kerr metric that describes rotating black holes in these theories. We express the solution as a series in the spin parameter χ, and we show that including enough terms in the expansion we are able to describe black holes with large spin. For the computations in the text we use an expansion up to order χ 14 , which is accurate for χ < 0.7, but we provide as well a Mathematica notebook that computes the solution at any given order. We study several properties of the corrected black holes, such as geometry of the horizon, ergosphere, light rings and scalar hair. Some of the corrections violate parity, and we highlight in those cases plots of horizons and ergospheres without Z 2 symmetry.

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Does a black hole rotate in Chern-Simons modified gravity?

Cited by 46 publications

References 20 publications

Thin accretion disk signatures in dynamical Chern–Simons-modified gravity

Thin accretion disk signatures in dynamical Chern–Simons-modified gravity

Quantum phase shift in Chern-Simons modified gravity

Leading higher-derivative corrections to Kerr geometry

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