Erratum: Quantization of the electromagnetic field outside static black holes and its application to low-energy phenomena [Phys. Rev. D<b>63</b>, 124008 (2001)]

Crispino, Luís C. B.; Higuchi, Atsushi; Matsas, George E. A.

doi:10.1103/physrevd.80.029906

Cited by 40 publications

(57 citation statements)

References 28 publications

Supporting

Mentioning

Contrasting

Unclassified

Order By: Relevance

“…On the other hand, our results are consistent with [32,33], where the issue was treated from a different perspective aiming quantum field theory applications. In order to make the discrepancies clear, and also to fix notation, we will review the approach in [31] and present our development in some detail.…”

Section: Electromagnetic Perturbationssupporting

confidence: 81%

Electromagnetic perturbations in new brane world scenarios

Molina¹,

Pavan²,

Torrejón³

2016

Phys. Rev. D

View full text Add to dashboard Cite

In this work we consider electromagnetic dynamics in Randall-Sundrum branes. It is derived a family of four-dimensional spacetimes compatible with Randall-Sundrum brane worlds, focusing on asymptotic flat backgrounds. Maximal extensions of the solutions are constructed and their causal structures are discussed. These spacetimes include singular, non-singular and extreme black holes. Maxwell's electromagnetic field is introduced and its evolution is studied in an extensive numerical survey. Electromagnetic quasinormal mode spectra are derived and analyzed with timedependent and high-order WKB methods. Our results indicate that the black holes in the brane are electromagnetically stable.

show abstract

Section: Electromagnetic Perturbationssupporting

confidence: 81%

Electromagnetic perturbations in new brane world scenarios

Molina¹,

Pavan²,

Torrejón³

2016

Phys. Rev. D

View full text Add to dashboard Cite

show abstract

“…Since the mode function of the spin-3/2 field will be represented by the spinor-vector wave functions, we have to do the construction analogous to the details with the spinor and the vector fields. In the study of Maxwell fields it has been shown that there are two physical modes with different mode functions [10,11]. One is related to the scalar spherical harmonics, and another one is related to the vector spherical harmonics, these are also known as the "longitudinal" and "transverse" parts of a vector field [12].…”

Section: The Radial Equation and The Potential Functionmentioning

confidence: 99%

Spin-3/2fields inD-dimensional Schwarzschild black hole spacetimes

et al. 2016

View full text Add to dashboard Cite

In previous works we have studied spin-3/2 fields near 4-dimensional Schwarzschild black holes.The techniques we developed in that case have now been extended here to show that it is possible to determine the potential of spin-3/2 fields near D-dimensional black holes by exploiting the radial symmetry of the system. This removes the need to use the Newman-Penrose formalism, which is difficult to extend to D-dimensional space-times. In this paper we will derive a general Ddimensional gauge invariant effective potential for spin-3/2 fields near black hole systems. We then use this potential to determine the quasi-normal modes and absorption probabilities of spin-3/2 fields near a D-dimensional Schwarzschild black hole.

show abstract

“…The Schwarzschild solution describes static and chargeless black holes, with event horizon at r h = 2M . The Lagrangian density of the electromagnetic field in the modified Feynman gauge is [20] …”

Section: Arxiv:09053339v1 [Gr-qc] 20 May 2009mentioning

confidence: 99%

Electromagnetic Wave Scattering by Schwarzschild Black Holes

2009

Self Cite

View full text Add to dashboard Cite

We analyze the scattering of a planar monochromatic electromagnetic wave incident upon a Schwarzschild black hole. We obtain accurate numerical results from the partial wave method for the electromagnetic scattering cross section, and show that they are in excellent agreement with analytical approximations. The scattering of electromagnetic waves is compared with the scattering of scalar, spinor and gravitational waves. We present a unified picture of the scattering of all massless fields for the first time.PACS numbers: 04.40.-b, 04.70.-s, 11.80.-m Black holes are thought to be efficient catalysts for the liberation of rest-mass energy. As such, black holes are implicated in the most energetic phenomena in the known universe (e.g. gamma ray bursts). On the other hand, after a turbulent youth, many black holes settle into a quiescent old age. Some estimates suggest there may be up to a billion quiescent stellar-mass black holes within our galaxy [1]. Their existence may be inferred from, for example, the transient lensing of background sources; a handful of events have so far been observed [2]. A possibility for future consideration is that quiescent black holes may be indirectly identified from the 'fingerprint' they leave on radiation that impinges upon them.Over the last four decades, some clues about the properties of any such 'fingerprint' have been uncovered. For example, a time-dependent perturbation incident upon a black hole will excite characteristic damped ringing in response. The frequencies and decay rates of the ringing are linked to the well-studied quasinormal mode spectrum [3]. Black holes illuminated by long-lasting planar radiation will create interference patterns, and rotating black holes will create distinctive polarization patterns [4]. Both effects depend strongly on the ratio of horizon size to wavelength. Hence, it is conceivable that future gravitational-wave detectors may be able to identify the fingerprint from rapid and distinctive variations across a narrow frequency band. Nevertheless, inferring the presence of quiescent black holes from such clues must remain a challenge for future decades.Scattering by black holes is of foundational interest in both black hole physics [5] and scattering theory [6]. Many authors have studied the simplest timeindependent scenario, in which a black hole is subject to a long-lasting, monochromatic beam of radiation. Here, the key dimensionless quantity is the ratio r h /λ where r h is the horizon size of the black hole, and λ is the wavelength of the incident wave. The interference pattern depends also on the spin s of the perturbing field, with s = 0, 1/2, 1 and 2 corresponding to scalar, neutrino, electromagnetic and gravitational fields, respectively.To the best of our knowledge, the first paper outlining a calculation of wave scattering cross section in the spacetime of a black hole was published by Matzner [7] in the late sixties. Since then, planar wave scattering from black holes has received much attention, especially in Schwarzschild and...

show abstract

Erratum: Quantization of the electromagnetic field outside static black holes and its application to low-energy phenomena [Phys. Rev. D63, 124008 (2001)]

Cited by 40 publications

References 28 publications

Electromagnetic perturbations in new brane world scenarios

Electromagnetic perturbations in new brane world scenarios

Spin-3/2fields inD-dimensional Schwarzschild black hole spacetimes

Electromagnetic Wave Scattering by Schwarzschild Black Holes

Contact Info

Product

Resources

About