Evidence for Electron-Hole Recombination Mechanism of Defect Production in KCl and NaCl at 20°K

Martel, P.; Hallett, A. C. Hollis

doi:10.1103/physrev.178.1437

Cited by 8 publications

(18 citation statements)

References 11 publications

Supporting

Mentioning

Contrasting

Order By: Relevance

“…This gives us a way of deducing the dominant, adiabatic evolution without actually resorting to a calculation of the local GSF. Computational methods for asymptotic fluxes in black-hole perturbation theory have been well developed since the early 1970s, and have been performed many times using frequency-domain methods (e.g, [144,147,145,146,148]) as well as time-domain ones [149,150,91,92,151]. Such calculations are much less computationally expensive than local GSF calculations, and can be done in the convenient framework of Teukolsky's perturbation formalism, working with Ψ 0 or Ψ 4 instead of the full metric perturbation.…”

Section: Balance Laws and Adiabatic Evolutionmentioning

confidence: 99%

Self-force and radiation reaction in general relativity

Barack¹,

Pound²

2018

Rep. Prog. Phys.

356

331

View full text Add to dashboard Cite

The detection of gravitational waves from binary black-hole mergers by the LIGO-Virgo Collaboration marks the dawn of an era when generalrelativistic dynamics in its most extreme manifestation is directly accessible to observation. In the future, planned (space-based) observatories operating in the millihertz band will detect the intricate gravitational-wave signals from the inspiral of compact objects into massive black holes residing in galactic centers. Such inspiral events are extremely effective probes of black-hole geometries, offering unparalleled precision tests of General Relativity in its most extreme regime. This prospect has in the past two decades motivated a programme to obtain an accurate theoretical model of the strong-field radiative dynamics in a two-body system with a small mass ratio. The problem naturally lends itself to a perturbative treatment based on a systematic expansion of the field equations in the small mass ratio. At leading order one has a pointlike particle moving in a geodesic orbit around the large black hole. At subsequent orders, interaction of the particle with its own gravitational perturbation gives rise to an effective "self-force", which drives the radiative evolution of the orbit, and whose effects can be accounted for order by order in the mass ratio.This review surveys the theory of gravitational self-force in curved spacetime and its application to the astrophysical inspiral problem. We first lay the relevant formal foundation, describing the rigorous derivation of the equation of self-forced motion using matched asymptotic expansions and other ideas. We then review the progress that has been achieved in numerically calculating the self-force and its physical effects in astrophysically realistic inspiral scenarios. We highlight the way in which, nowadays, self-force calculations make a fruitful contact with other approaches to the two-body problem and help inform an accurate universal model of binary black hole inspirals, valid across all mass ratios. We conclude with a summary of the state of the art, open problems and prospects.Our review is aimed at non-specialist readers and is for the most part selfcontained and non-technical; only elementary-level acquaintance with General Relativity is assumed. Where useful, we draw on analogies with familiar concepts from Newtonian gravity or classical electrodynamics. 7

show abstract

Section: Balance Laws and Adiabatic Evolutionmentioning

confidence: 99%

Self-force and radiation reaction in general relativity

Barack¹,

Pound²

2018

Rep. Prog. Phys.

356

331

View full text Add to dashboard Cite

show abstract

“…At present, in the case of non-rotating black holes the metric perturbative scheme is completely developed and well understood at the linear level (see [27,28,29,30,31,32,33] for reviews). In the particular case of perturbations induced by an orbiting point-like object, which is the situation we are interested in this paper, there are a number of works on it [32,34,35,36,37,38,39]. Here, we summarize the theory using a particular formulation that makes the different expressions involved compact and self-explanatory.…”

Section: Summary Of Perturbation Theory For Non-rotating Black Holesmentioning

confidence: 99%

Finite element computation of the gravitational radiation emitted by a pointlike object orbiting a nonrotating black hole

Sopuerta

Laguna

2006

Phys. Rev. D

View full text Add to dashboard Cite

The description of extreme-mass-ratio binary systems in the inspiral phase is a challenging problem in gravitational wave physics with significant relevance for the space interferometer LISA. The main difficulty lies in the evaluation of the effects of the small body's gravitational field on itself. To that end, an accurate computation of the perturbations produced by the small body with respect the background geometry of the large object, a massive black hole, is required. In this paper we present a new computational approach based on Finite Element Methods to solve the master equations describing perturbations of non-rotating black holes due to an orbiting point-like object. The numerical computations are carried out in the time domain by using evolution algorithms for wave-type equations. We show the accuracy of the method by comparing our calculations with previous results in the literature. Finally, we discuss the relevance of this method for achieving accurate descriptions of extreme-mass-ratio binaries.

show abstract

“…On the one hand, for quasicircular, comparable mass BH inspirals, the effect of these fluxes on the GW phase amounts to less than one radian for an event in the LIGO frequency band [8]. On the other hand, for quasicircular, extreme mass-ratio inspirals, such tidal effects can increase the duration of the signal up to 20 days in two years for an event in the frequency band of a space-borne detector [11][12][13]. For eccentric and inclined extreme mass ratio inspirals (EMRIs), this effect could be even larger [14][15][16].…”

Section: Introductionmentioning

confidence: 99%

Tidal heating and torquing of a Kerr black hole to next-to-leading order in the tidal coupling

2013

View full text Add to dashboard Cite

We calculate the linear vacuum perturbations of a Kerr black hole surrounded by a slowly varying external spacetime to third order in the ratio of the black-hole mass to the radius of curvature of the external spacetime. This expansion applies to two relevant physical scenarios: (i) a small Kerr black hole immersed in the gravitational field of a much larger external black hole, and (ii) a Kerr black hole moving slowly around another external black hole of comparable mass. This small-hole/slow-motion approximation allows us to parametrize the perturbation through slowly varying, time-dependent electric and magnetic tidal tensors, which then enable us to separate the Teukolsky equation and compute the Newman-Penrose scalar analytically to third order in our expansion parameter. We obtain generic expressions for the mass and angular momentum flux through the perturbed black hole horizon, as well as the rate of change of the horizon surface area, in terms of certain invariants constructed from the electric and magnetic tidal tensors. We conclude by applying these results to the second scenario described above.

show abstract

Evidence for Electron-Hole Recombination Mechanism of Defect Production in KCl and NaCl at 20°K

Cited by 8 publications

References 11 publications

Self-force and radiation reaction in general relativity

Self-force and radiation reaction in general relativity

Finite element computation of the gravitational radiation emitted by a pointlike object orbiting a nonrotating black hole

Tidal heating and torquing of a Kerr black hole to next-to-leading order in the tidal coupling

Contact Info

Product

Resources

About