Evolution of radiating charged spheres in general relativity

1988 ◽  
Vol 66 (11) ◽  
pp. 981-986 ◽  
Author(s):  
V. Medina ◽  
L. Núñez ◽  
H. Rago ◽  
A. Patiño
Keyword(s):  
General Relativity ◽  
Energy Density ◽  
Radial Velocity ◽  
Maxwell Equations ◽  
Charged Fluid ◽  
Vaidya Solution ◽  
Physical Variables ◽  
Electric Charge Distribution ◽  
Fluid Spheres ◽  
Charged Spheres

A method reported by Herrera et al. is extended to study radiating, charged, fluid spheres. A heuristic assumption relating pressure, energy density, the radial velocity of matter, and the electric-charge distribution is introduced. This ansatz, together with matching the boundaries with those of the Reissner–Nordstrom–Vaidya solution, leads to a system of ordinary differential equations for quantities evaluated at the surface. The integration allows one to obtain the profile of the physical variables for any piece of material via the Einstein–Maxwell equations. As an example of the procedure, a particular model is worked out in some detail.

Some static relativistic compact charged fluid spheres in general relativity

2013 ◽  
Vol 350 (1) ◽  
pp. 293-305 ◽  
Author(s):  
Mohammad Hassan Murad ◽  
Saba Fatema
Keyword(s):  
General Relativity ◽  
Charged Fluid ◽  
Fluid Spheres

Charged spheres in general relativity

1969 ◽  
Vol 47 (18) ◽  
pp. 1989-1994 ◽  
Author(s):  
M. C. Faulkes
Keyword(s):  
General Relativity ◽  
Total Energy ◽  
General Equation ◽  
Maxwell Equations ◽  
Equilibrium Configuration ◽  
Rate Of Change ◽  
Spherically Symmetric ◽  
Charged Matter ◽  
Spherically Symmetric Distribution ◽  
Charged Spheres

The Einstein–Maxwell equations for a spherically symmetric distribution of charged matter are studied. A general equation is derived for the rate of change of the "total energy" of the sphere in terms of the 4–4 component of the electromagnetic and matter tensors. It is shown that, subject to certain conditions, the spheres of charged matter can oscillate, and further that the static configuration is uniquely given by the relation m2 = 4πe2α, where [Formula: see text]. Finally, it is demonstrated that the equilibrium configuration is unstable to small radial perturbations.

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.

Slowly rotating charged fluid spheres in general relativity

1986 ◽  
Vol 34 (2) ◽  
pp. 327-330 ◽  
Author(s):  
R. N. Tiwari ◽  
J. R. Rao ◽  
R. R. Kanakamedala
Keyword(s):  
General Relativity ◽  
Charged Fluid ◽  
Fluid Spheres

scholarly journals ISOTROPIC CASES OF STATIC CHARGED FLUID SPHERES IN GENERAL RELATIVITY

2011 ◽  
Vol 20 (09) ◽  
pp. 1675-1687 ◽  
Author(s):  
BASANTI DAS ◽  
PRATAP CHANDRA RAY ◽  
IRINA RADINSCHI ◽  
FAROOK RAHAMAN ◽  
SAIBAL RAY
Keyword(s):  
General Relativity ◽  
Analytical Solutions ◽  
Density Ratio ◽  
Compact Stars ◽  
Maxwell Field ◽  
Field Equations ◽  
Charged Fluid ◽  
Isotropic Coordinates ◽  
Charged Fluid Sphere ◽  
Fluid Spheres

In this paper we study the isotropic cases of static charged fluid spheres in general relativity. For this purpose we consider two different specializations and under these we solve the Einstein–Maxwell field equations in isotropic coordinates. The analytical solutions thus obtained are matched to the exterior Reissner–Nordström solutions which concern the values for the metric coefficients eν and eμ. We derive the pressure, density and pressure-to-density ratio at the center of the charged fluid sphere and boundary R of the star. Our conclusion is that static charged fluid spheres provide a good connection to compact stars.

Three new exact solutions for charged fluid spheres in general relativity

2014 ◽  
Vol 356 (1) ◽  
pp. 75-87 ◽  
Author(s):  
S. K. Maurya ◽  
Y. K. Gupta ◽  
Baiju Dayanandan ◽  
T. T. Smitha
Keyword(s):  
General Relativity ◽  
Exact Solutions ◽  
Charged Fluid ◽  
New Exact Solutions ◽  
Fluid Spheres

Cylindrical waves in general relativity

1986 ◽  
Vol 408 (1835) ◽  
pp. 209-232 ◽  
Keyword(s):  
General Relativity ◽  
Gravitational Field ◽  
Energy Density ◽  
Perfect Fluid ◽  
Maxwell Equations ◽  
Cylindrical Symmetry ◽  
Hamiltonian Density ◽  
Cylindrical Waves ◽  
Cylindrically Symmetric ◽  
Set Up

A convenient framework is set up for constructing cylindrically symmetric solutions of the Einstein and the Einstein—Maxwell equations, and it is shown how a Hamiltonian density can be defined for space-times with cylindrical symmetry. Solutions are obtained that represent stationary monochromatic waves and satisfy all the requisite conditions of regularity. The case when the gravitational field is coupled with a perfect fluid in which the energy density is equal to the pressure is also briefly considered.

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