scholarly journals Black Plane Solutions and Localized Gravitational Energy

2015 ◽  
Vol 2015 ◽  
pp. 1-4
Author(s):  
Paul Halpern ◽  
Jennifer Roberts
Keyword(s):  
Energy Distribution ◽  
Maxwell Equations ◽  
Gravitational Energy ◽  
De Sitter ◽  
Energy Localization ◽  
Energy Distributions ◽  
Plane Symmetric ◽  
Static Plane ◽  
Black Plane

We explore the issue of gravitational energy localization for static plane-symmetric solutions of the Einstein-Maxwell equations in 3+1 dimensions with asymptotic anti-de Sitter behavior. We apply three different energy-momentum complexes, the Einstein, Landau-Lifshitz, and Møller prescriptions, to the metric representing this category of solutions and determine the energy distribution for each. We find that the three prescriptions offer identical energy distributions, suggesting their utility for this type of model.

scholarly journals ENERGY DISTRIBUTION OF BLACK PLANE SOLUTIONS

2006 ◽  
Vol 21 (06) ◽  
pp. 495-502 ◽  
Author(s):  
PAUL HALPERN
Keyword(s):  
Energy Distribution ◽  
Cosmological Constant ◽  
Electric Charge ◽  
Maxwell Equations ◽  
De Sitter ◽  
Plane Symmetric ◽  
Sitter Solution ◽  
Static Plane ◽  
Momentum Complex ◽  
Black Plane

We use the Einstein energy–momentum complex to calculate the energy distribution of static plane-symmetric solutions of the Einstein–Maxwell equations in 3+1 dimensions with asymptotic anti-de Sitter behavior. This solution is expressed in terms of three parameters: the mass, electric charge and cosmological constant. We compare the energy distribution to that of the Reissner–Nordström–anti-de Sitter solution, pointing to qualitative differences between the models. Finally, we examine these results within the context of the Cooperstock hypothesis.

scholarly journals ON ENERGY DISTRIBUTION OF TWO SPACE–TIMES WITH PLANAR AND CYLINDRICAL SYMMETRIES

2009 ◽  
Vol 24 (04) ◽  
pp. 789-797 ◽  
Author(s):  
SAEED MIRSHEKARI ◽  
AMIR M. ABBASSI
Keyword(s):  
Energy Distribution ◽  
Maxwell Equations ◽  
Spherically Symmetric ◽  
Plane Symmetric ◽  
Cylindrically Symmetric ◽  
Symmetric Metrics ◽  
Static Plane

Considering encouraging Virbhadra results about energy distribution of nonstatic spherically symmetric metrics in the Kerr–Schild class, it would be interesting to study some space–times with other symmetries. Using Møller and Einstein energy–momentum complexes in static plane-symmetric and cylindrically symmetric solutions to Einstein–Maxwell equations in 3+1 dimensions, energy (due to matter and fields including gravity) distribution is studied. Energy expressions are obtained finite and well-defined. Our results support the Cooperstock hypothesis about localized energy.

scholarly journals The Localized Energy Distribution of Dark Energy Star Solutions

2013 ◽  
Vol 2013 ◽  
pp. 1-4 ◽  
Author(s):  
Paul Halpern ◽  
Michael Pecorino
Keyword(s):  
Exact Solution ◽  
Dark Energy ◽  
Scalar Field ◽  
Energy Distribution ◽  
Phantom Energy ◽  
Energy Localization ◽  
Einstein’S Equations ◽  
Energy Distributions ◽  
Einstein's Equations ◽  
Energy Star

We examine the question of energy localization for an exact solution of Einstein's equations with a scalar field corresponding to the phantom energy interpretation of dark energy. We apply three different energy-momentum complexes, the Einstein, the Papapetrou, and the Møller prescriptions, to the exterior metric and determine the energy distribution for each. Comparing the results, we find that the three prescriptions yield identical energy distributions.

General static plane-symmetric solutions of the Einstein-Maxwell equations

1983 ◽  
Vol 27 (8) ◽  
pp. 1731-1739 ◽  
Author(s):  
P. A. Amundsen ◽  
Ø. Grøn
Keyword(s):  
Maxwell Equations ◽  
Plane Symmetric ◽  
Static Plane

Null Fluid Collapse in the Plane Symmetric Anti-de Sitter Spacetime

1997 ◽  
Vol 12 (03) ◽  
pp. 155-161 ◽  
Author(s):  
Rong-Gen Cai ◽  
Ling-Zhi Qiao ◽  
Yuan-Zhong Zhang
Keyword(s):  
Exact Solution ◽  
Late Time ◽  
De Sitter Spacetime ◽  
De Sitter ◽  
Curvature Singularity ◽  
Plane Symmetric ◽  
Sitter Spacetime ◽  
Plane Solution ◽  
The Stability ◽  
Black Plane

The stability of the plane anti-de Sitter spacetime and the gravitational collapse in the plane symmetric anti-de Sitter spacetime are investigated. A scalar curvature singularity will be formed at the r=0 plane when the anti-de Sitter spacetime is perturbed by null dust. By employing the method suggested recently by Husain we find a family of non-static exact solution of the null fluid collapse with equation of state P=kρ in the plane anti-de Sitter spacetime. The late time limit of the solutions results in a black plane solution possessing multiple horizon structure.

Intelligent Gear Fault Identification Method Based on Harmonic Wavelet Package Energy Distribution and Grey Incidence

2013 ◽  
Vol 694-697 ◽  
pp. 1155-1159
Author(s):  
Wen Bin Zhang ◽  
Yan Ping Su ◽  
Yan Jie Zhou ◽  
Ya Song Pu
Keyword(s):  
Energy Distribution ◽  
Fault Identification ◽  
Morphological Filter ◽  
Original Signal ◽  
Energy Distributions ◽  
Vibration Signals ◽  
Fault Pattern ◽  
Gear Fault ◽  
Harmonic Wavelet ◽  
Gear Fault Diagnosis

In this paper, a novel intelligent method to identify gear fault pattern was approached based on morphological filter, harmonic wavelet package and grey incidence. At first, the line structure element was selected for morphological filter to denoise the original signal. Secondly, different gear fault signals were decomposed into eight frequency bands by harmonic wavelet package in three levels; and energy distribution of each band was calculated. Finally, these energy distributions could serve as the feature vectors, the grey incidence of different gear vibration signals was calculated to identify the fault pattern and condition. Practical results show that this method can be used in gear fault diagnosis effectively.

scholarly journals f(T) gravity and energy distribution in Landau–Lifshitz prescription

2018 ◽  
Vol 27 (04) ◽  
pp. 1850039 ◽  
Author(s):  
M. G. Ganiou ◽  
M. J. S. Houndjo ◽  
J. Tossa
Keyword(s):  
General Relativity ◽  
Energy Density ◽  
Energy Distribution ◽  
Cosmic String ◽  
Mass Formula ◽  
Plane Symmetric ◽  
Symmetric Metrics ◽  
Teleparallel Theory ◽  
Momentum Complex ◽  
Theory View

We investigate in this paper the Landau–Lifshitz energy distribution in the framework of [Formula: see text] theory view as a modified version of Teleparallel theory. From some important Teleparallel theory results on the localization of energy, our investigations generalize the Landau–Lifshitz prescription from the computation of the energy–momentum complex to the framework of [Formula: see text] gravity as it is done in the modified versions of General Relativity. We compute the energy density in the first step for three plane-symmetric metrics in vacuum. We find for the second metric that the energy density vanishes independently of [Formula: see text] models. We find that the Teleparallel Landau–Lifshitz energy–momentum complex formulations for these metrics are different from those obtained in General Relativity for the same metrics. Second, the calculations are performed for the cosmic string spacetime metric. It results that the energy distribution depends on the mass [Formula: see text] and the radius [Formula: see text] of cosmic string and it is strongly affected by the parameter of the considered quadratic and cubic [Formula: see text] models. Our investigation with this metric induces interesting results susceptible to be tested with some astrophysics hypothesis.

scholarly journals Energy distribution in globular star clusters

1964 ◽  
Vol 20 ◽  
pp. 358-370
Author(s):  
L. H. Aller ◽  
D. J. Faulkner
Keyword(s):  
Energy Distribution ◽  
Spectral Range ◽  
Globular Clusters ◽  
Broad Band ◽  
Star Clusters ◽  
The Other ◽  
Energy Distributions ◽  
Single Observation ◽  
Band Pass ◽  
Time Required

The present investigation is concerned with the energy distributions in globular clusters. In a sense, energy-distribution measurements are comparable with multi-colour photometry. The chief advantage is that narrower band-passes may be used and the entire spectrum traced, whereas in multi-colour photometry one is limited to effective wavelengths determined by the filter and a rather broad band-pass. On the other hand, broad band-pass photometry often permits one to cover a broader spectral range, and to work much faster. Since the time required for a single observation is much shorter, the observer is less at the mercy of the sky transparency. Hence a greater accuracy can be obtained.

scholarly journals Broad-band study of high-synchrotron-peaked BL Lac object 1ES 1218+304

2020 ◽  
Vol 496 (4) ◽  
pp. 5518-5527
Author(s):  
N Sahakyan
Keyword(s):  
Energy Distribution ◽  
Electron Energy ◽  
Power Law ◽  
Spectral Energy Distribution ◽  
Broad Band ◽  
Energy Distributions ◽  
X Ray ◽  
Bl Lac ◽  
Photon Index ◽  
Γ Ray

ABSTRACT The origin of the multiwavelength emission from the high-synchrotron-peaked BL Lac 1ES 1218+304 is studied using the data from SwiftUVOT/XRT, NuSTAR, and Fermi-LAT. A detailed temporal and spectral analysis of the data observed during 2008–2020 in the  γ-ray (>100 MeV), X-ray (0.3–70 keV), and optical/UV bands is performed. The γ-ray spectrum is hard with a photon index of 1.71 ± 0.02 above 100 MeV. The SwiftUVOT/XRT data show a flux increase in the UV/optical and X-ray bands; the highest 0.3–3 keV X-ray flux was (1.13 ± 0.02) × 10−10 erg cm−2 s−1. In the 0.3–10 keV range, the averaged X-ray photon index is >2.0 which softens to 2.56 ± 0.028 in the 3–50 keV band. However, in some periods, the X-ray photon index became extremely hard (<1.8), indicating that the peak of the synchrotron component was above 1 keV, and so 1ES 1218+304 behaved like an extreme synchrotron BL Lac. The hardest X-ray photon index of 1ES 1218+304 was 1.60 ± 0.05 on MJD 58489. The time-averaged multiwavelength spectral energy distribution is modelled within a one-zone synchrotron self-Compton leptonic model using a broken power law and power law with an exponential cutoff electron energy distributions. The data are well explained when the electron energy distribution is $E_{\rm e}^{-2.1}$ extending up to γbr/cut ≃ (1.7 − 4.3) × 105, and the magnetic field is weak (B ∼ 1.5 × 10−2 G). By solving the kinetic equation for electron evolution in the emitting region, the obtained electron energy distributions are discussed considering particle injection, cooling, and escape.

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