Charge effects in a static, spherically symmetric, gravitating fluid

Olson, E.; Bailyn, M.

doi:10.1103/physrevd.13.2204

Cited by 36 publications

(37 citation statements)

References 5 publications

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“…Furthermore, as shown by Bekenstein [14] the electric charge is bounded by the fact that the resulting electric field should not exceed the critical field for pair creation, 10 16 V cm −1 . However, these restrictions have been questioned by several authors [15,18,20,37]. Particularly appealing is the possibility of very high electric fields in strange stars with quark matter (see [38,39] and references therein).…”

Section: Introductionmentioning

confidence: 99%

Nonadiabatic charged spherical gravitational collapse

et al. 2007

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We present a complete set of the equations and matching conditions required for the description of physically meaningful charged, dissipative, spherically symmetric gravitational collapse with shear. Dissipation is described with both free-streaming and diffusion approximations. The effects of viscosity are also taken into account. The roles of different terms in the dynamical equation are analyzed in detail. The dynamical equation is coupled to a causal transport equation in the context of Israel-Stewart theory. The decrease of the inertial mass density of the fluid, by a factor which depends on its internal thermodynamic state, is reobtained, with the viscosity terms included. In accordance with the equivalence principle, the same decrease factor is obtained for the gravitational force term. The effect of the electric charge on the relation between the Weyl tensor and the inhomogeneity of energy density is discussed.2

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Section: Introductionmentioning

confidence: 99%

Nonadiabatic charged spherical gravitational collapse

et al. 2007

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“…The internal electric field of an astronomical object can be very large in some special scenarios [46], [28], [29], [39]. In particular, the charge separation inside a spherical compact star, in hydrostatic equilibrium, can be very large when one of the plasma components is a degenerate gas while the other is a Maxwell-Boltzmann gas, i.e., like the gas of degenerated electrons and the gas of nuclei in a white dwarf [29].…”

Section: Introductionmentioning

confidence: 99%

Numeric simulation of relativistic stellar core collapse and the formation of Reissner-Nordström black holes

Ghezzi

Letelier

2007

Phys. Rev. D

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The time evolution of a set of 22M⊙ unstable charged stars that collapse is computed integrating the Einstein-Maxwell equations. The model simulate the collapse of an spherical star that had exhausted its nuclear fuel and have or acquires a net electric charge in its core while collapsing. When the charge to mass ratio is Q/ √ GM ≥ 1 the star do not collapse and spreads. On the other hand, it is observed a different physical behavior with a charge to mass ratio 1 > Q/ √ GM > 0.1. In this case, the collapsing matter forms a bubble enclosing a lower density core. We discuss an immediate astrophysical consequence of these results that is a more efficient neutrino trapping during the stellar collapse and an alternative mechanism for powerful supernova explosions. The outer space-time of the star is the Reissner-Nordström solution that match smoothly with our interior numerical solution, thus the collapsing models forms Reissner-Nordström black holes.

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“…Therefore, the overall system outside each WS cell is strictly neutral and no global electric field exists, contrary to previous results reported in literature. 20 The value of the critical mass and the radius of the white dwarf in our treatment and in the Hamada and Salpeter 19 treatment becomes a function of the nuclear composition of the star. The mass-radius relation of Chandrasekhar, of Hamada & Salpeter and ours have been compared and contrasted in the case of 4 He, 12 C, 16 O and 56 Fe nuclear compositions 15 (see e.g.…”

Section: The Relativistic Fmt Treatment and General Relativistic Non-mentioning

confidence: 81%