Symmetry mappings in Einstein-Maxwell space-times

1979 ◽  
Vol 10 (1) ◽  
pp. 61-77 ◽  
Author(s):  
C. B. G. McIntosh
Keyword(s):  
Maxwell Space

The Einstein pseudo-tensor and the flux integral for perturbed static space-times

1991 ◽  
Vol 435 (1895) ◽  
pp. 645-657 ◽  
Keyword(s):  
Energy Momentum Tensor ◽  
Momentum Tensor ◽  
Einstein Equations ◽  
Second Variation ◽  
Common Procedure ◽  
Static Vacuum ◽  
Linear Perturbations ◽  
Maxwell Space ◽  
The Common ◽  
Static Space

The flux integral for axisymmetric polar perturbations of static vacuum space-times, derived in an earlier paper directly from the relevant linearized Einstein equations, is rederived with the aid of the Einstein pseudo-tensor by a simple algorism. A similar earlier effort with the aid of the Landau–Lifshitz pseudo-tensor failed. The success with the Einstein pseudo-tensor is due to its special distinguishing feature that its second variation retains its divergence-free property provided only the equations governing the static space-time and its linear perturbations are satisfied. When one seeks the corresponding flux integral for Einstein‒Maxwell space-times, the common procedure of including, together with the pseudo-tensor, the energy‒momentum tensor of the prevailing electromagnetic field fails. But, a prescription due to R. Sorkin, of including instead a suitably defined ‘Noether operator’, succeeds.

scholarly journals Study of charged compact stars with class 1 metric under general relativity

2019 ◽  
Vol 97 (12) ◽  
pp. 1323-1331 ◽  
Author(s):  
S.K. Maurya ◽  
S. Roy Chowdhury ◽  
Saibal Ray ◽  
B. Dayanandan
Keyword(s):  
General Relativity ◽  
Compact Star ◽  
Space Time ◽  
Electron Cloud ◽  
Compact Stars ◽  
Stellar Structure ◽  
Spherically Symmetric ◽  
Class 1 ◽  
Maxwell Space ◽  
Physical Tests

In the present paper we study compact stars under the background of Einstein–Maxwell space–time, where the 4-dimensional spherically symmetric space–time of class 1 along with the Karmarkar condition has been adopted. The investigations, via the set of exact solutions, show several important results, such as (i) the value of density on the surface is finite; (ii) due to the presence of the electric field, the outer surface or the crust region can be considered to be made of electron cloud; (iii) the charge increases rapidly after crossing a certain cutoff region (r/R ≈ 0.3); and (iv) the avalanche of charge has a possible interaction with the particles that are away from the center. As the stellar structure supports all the physical tests performed on it, therefore the overall observation is that the model provides a physically viable and stable compact star.

Infinitesimal holonomy groups of Einstein-Maxwell space-times

1987 ◽  
Vol 19 (1) ◽  
pp. 95-107 ◽  
Author(s):  
C. D. Collinson ◽  
P. N. Smith
Keyword(s):  
Holonomy Groups ◽  
Maxwell Space

The infinitesimal holonomy group structure of EEnstein-Maxwell space-times

1979 ◽  
Vol 53 (2) ◽  
pp. 209-232 ◽  
Author(s):  
L. K. Norris ◽  
W. R. Davis
Keyword(s):  
Group Structure ◽  
Holonomy Group ◽  
Maxwell Space

The flux integral for axisymmetric perturbations of static space-times

1990 ◽  
Vol 428 (1875) ◽  
pp. 325-349 ◽  
Keyword(s):  
Black Holes ◽  
Perfect Fluid ◽  
Gravitational Radiation ◽  
Scattering Theory ◽  
Scattering Matrix ◽  
Conservation Of Energy ◽  
Fluid Source ◽  
Maxwell Space ◽  
Static Space ◽  
Axisymmetric Perturbations

The axisymmetric perturbations of static space-times with prevailing sources (a Maxwell field or a perfect fluid) are considered; and it is shown how a flux integral can be derived directly from the relevant linearized equations. The flux integral ensures the conservation of energy in the attendant scattering of radiation and the sometimes accompanying transformation of one kind of radiation into another. The flux integral derived for perturbed Einstein-Maxwell space-times will be particularly useful in this latter context (as in the scattering of radiation by two extreme Reissner-Nordström black-holes) and in the setting up of a scattering matrix. And the flux integral derived for a space-time with a perfect-fluid source will be directly applicable to the problem of the non-radial oscillations of a star with accompanying emission of gravitational radiation and enable its reformulation as a problem in scattering theory.

Holonomy transformation and Aharonov-Bohm effect in an Einstein-Maxwell space-time

1988 ◽  
Vol 38 (2) ◽  
pp. 506-508 ◽  
Author(s):  
V. B. Bezerra
Keyword(s):  
Space Time ◽  
Maxwell Space ◽  
Bohm Effect ◽  
Aharonov Bohm

scholarly journals Static Einstein–Maxwell space-time invariant by translation

2021 ◽  
Vol 53 (10) ◽  
Author(s):  
Benedito Leandro ◽  
Ana Paula de Melo ◽  
Ilton Menezes ◽  
Romildo Pina
Keyword(s):  
Space Time ◽  
Maxwell Space ◽  
Time Invariant

Einstein-Maxwell space-times with symmetries and with non-null electromagnetic fields

1978 ◽  
Vol 9 (4) ◽  
pp. 277-288 ◽  
Author(s):  
C. B. G. McIntosh
Keyword(s):  
Electromagnetic Fields ◽  
Maxwell Space

scholarly journals The structure of groups of motions admitted by Einstein-Maxwell space-times

1973 ◽  
Vol 31 (1) ◽  
pp. 75-81 ◽  
Author(s):  
M. L. Woolley
Keyword(s):  
Maxwell Space

scholarly journals PHYSICAL PROPERTIES OF TOLMAN–BAYIN SOLUTIONS: SOME CASES OF STATIC CHARGED FLUID SPHERES IN GENERAL RELATIVITY

2007 ◽  
Vol 16 (11) ◽  
pp. 1745-1759 ◽  
Author(s):  
SAIBAL RAY ◽  
BASANTI DAS ◽  
FAROOK RAHAMAN ◽  
SUBHARTHI RAY
Keyword(s):  
General Relativity ◽  
Physical Properties ◽  
Perfect Fluid ◽  
Mass Density ◽  
Fluid Pressure ◽  
Matter Distribution ◽  
Electromagnetic Mass ◽  
Charged Fluid ◽  
Maxwell Space ◽  
Fluid Spheres

In this article, Einstein–Maxwell space–time is considered in connection with some of the astrophysical solutions previously obtained by Tolman (1939) and Bayin (1978). The effect of inclusion of charge in these solutions is investigated thoroughly and the nature of fluid pressure and mass density throughout the sphere is discussed. Mass–radius and mass–charge relations are derived for various cases of the charged matter distribution. Two cases are obtained where perfect fluid with positive pressures gives rise to electromagnetic mass models such that gravitational mass is of purely electromagnetic origin.

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