Compact objects in general relativity: From Buchdahl stars to quasiblack holes

Lemos, José P. S.; Заславский, О. Б.

doi:10.1142/s0218271820410199

Cited by 11 publications

(7 citation statements)

References 74 publications

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“…Since the pressure diverges the spacetime of nonextremal shells at R = r + presents some type of singularity. This singularity is mild however, with entropy and the mass formulas being derived in this limiting case, see [37]. The Carter-Penrose diagram of a nonextremal quasiblack hole is similar to the Carter-Penrose diagram for a Majumdar-Papapetrou one, i.e., the one showed in Figure 21.…”

Section: Majumdar-papapetrou Shell Quasiblack Holesmentioning

confidence: 73%

“…In this case a horizon is barely formed, namely, we have a quasihorizon, and so, following the nomenclature, r + is both the gravitational radius and the quasihorizon radius. This is an extremal quasiblack hole [37]. Also r + and r − have the same value.…”

Section: Majumdar-papapetrou Shell Quasiblack Holesmentioning

confidence: 81%

“…The Carter-Penrose diagram can be drawn with some care from the building blocks of an interior Minkowski spacetime and the exterior asymptotic region of an extremal Reissner-Nordström spacetime, see [31] and for more details see [37]. In Figure 21 the Carter-Penrose diagram of a Majumdar-Papapetrou shell quasiblack hole, i.e., for R = r + and a junction surface with orientation such that the outside normal points towards spacial infinity is shown.…”

Section: Majumdar-papapetrou Shell Quasiblack Holesmentioning

confidence: 99%

“…The study of spherically symmetric electrically charged thin shells with a Reissner-Nordström spacetime exterior was dealt by de la Cruz and Israel [18] and Kuchař [19], gravitational collapse of electrically charged shells was performed by Chase [20] and Boulware [21], Vilenkin and Fomin [22] inspected the problem of the self-energy of the electron through thin shells, the topology of the collapse of charged thin shells and fluids was analyzed by Hiscock [23], interacting electric thin shells were studied in Lemos and Zanchin, [24], Dias, Gao, and Lemos studied electric collapsing shells in Lovelock theory [25] with the general relativistic counterpart and its relation to cosmic censorship studied by Gao and Lemos [26], properties of highly compact electric shells together with their energy conditions where a maximum bound, of the kind of the Buchdahl bound has been found, have been discussed by Andréasson [27], the inclusion of a Vlasov fluid into a thin shell was studied by Andréasson, Eklund, and Rein [28], thin shell electrically charged wormholes were constructed by Dias and Lemos [29], regular black holes with thin shells were worked out in [30], the highest compact shells were analyzed by Lemos and Zaslavskii [31], Berezin and Dokuchaev performed a thorough study of gravitational collapse of electric thin shells [32], and properties of black holes, such as black hole entropy, through thin shells, were analyzed by Lemos, Quinta, and Zaslavskii [33,34], tension electric shells on the other side of the Reissner-Nordstöm universe were studied by Luz and Lemos [35], further study on thin shells with matter obeying the Einstein-Maxwell equations with the inclusion of a Vlasov fluid were analyzed in [36], and for the highest compact electric thin shells that form quasiblack holess see the work of Lemos and Zaslavskii [37].…”

Section: Introductionmentioning

confidence: 99%

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All fundamental electrically charged thin shells in general relativity: From star shells to tension shell black holes and regular black holes and beyond

Lemos,

Luz

2021

Preprint

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We classify all fundamental electrically charged thin shells in general relativity, i.e., static spherically symmetric perfect fluid thin shells with a Minkowski spacetime interior and a Reissner-Nordström spacetime exterior, characterized by the spacetime mass M , which we assume positive, and the electric charge Q, which without loss of generality in our analysis can always be assumed as being the modulus of the electric charge, be it positive or negative. The fundamental shell can exist in three states, namely, nonextremal when Q M < 1, which includes the Schwarzschild Q M = 0 state, extremal when Q M = 1, and overcharged when Q M > 1. The nonextremal state, Q M < 1, allows the shell to be located in such a way that the radius R of the shell can be outside its own gravitational radius r+, i.e., R > r+, where r+ is given in terms of M and Q by r+ = M + M 2 − Q 2 , or can be inside its own Cauchy radius r−, i.e., R < r−, where r− is given in terms of M and Q, allows the shell to be located in such a way that the radius R of the shell can be outside its own gravitational radius r+, i.e., R > r+, where now r+ = r−, or can be inside its own gravitational radius, i.e., R < r+, or can be at its own gravitational radius r+, i.e., R = r+. The overcharged state, Q M > 1, allows the shell to be located anywhere R ≥ 0. There is yet a further division, indeed, one has still to specify the orientation of the shell, i.e., whether the normal out of the shell points toward increasing radii or toward decreasing radii. For the shell's orientation, the analysis in the nonextremal state is readily performed using Kruskal-Szekeres coordinates, whereas in the extremal and overcharged states the analysis can be performed in the usual spherical coordinates. There is still a subdivision in the extremal state r+ = r− when the shell is at r+, R = r+, in that the shell can approach r+ from above or approach r+ from below. The shell is assumed to be composed of an electrically charged perfect fluid characterized by the energy density, pressure, and electric charge density, for which an analysis of the energy conditions, null, weak, dominant, and strong, is performed. In addition, the shell spacetime has a corresponding Carter-Penrose diagram that can be built out of the diagrams for Minkowski and Reissner-Nordström spacetimes. Combining these two characterizations, specifically, the physical properties and the Carter-Penrose diagrams, one finds that there are fourteen cases that comprise a bewildering variety of shell spacetimes, namely, nonextremal star shells, nonextremal tension shell black holes, nonextremal tension shell regular and nonregular black holes, nonextremal compact shell naked singularities, Majumdar-Papapetrou star shells, extremal tension shell singularities, extremal tension shell regular and nonregular black holes, Majumdar-Papapetrou compact shell naked singularities, Majumdar-Papapetrou shell quasiblack holes, extremal null shell quasinonblack holes, extremal null shell singularities, Majumdar-Papapetrou null shell si...

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Section: Majumdar-papapetrou Shell Quasiblack Holesmentioning

confidence: 73%

Section: Majumdar-papapetrou Shell Quasiblack Holesmentioning

confidence: 81%

Section: Majumdar-papapetrou Shell Quasiblack Holesmentioning

confidence: 99%

Section: Introductionmentioning

confidence: 99%

See 2 more Smart Citations

All fundamental electrically charged thin shells in general relativity: From star shells to tension shell black holes and regular black holes and beyond

Lemos,

Luz

2021

Preprint

Self Cite

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“…C 2 of Ref. [71] (see [72] for a recent short review), the whole region 0 ≤ r < a becomes an infinite redshift region and the surface a → m forms a quasi-horizon, characterizing a quasiblack hole configuration.…”

Section: The Line C3 R−/r = A/rmentioning

confidence: 99%

New regular black hole solutions and other electrically charged compact objects with a de Sitter core and a matter layer

Masa

Oliveira

Zanchin

2018

Int. J. Mod. Phys. D

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The main objective of this work is the construction of regular black hole solutions in the context of the Einstein–Maxwell theory. The strategy is to match an interior regular solution to an exterior electrovacuum solution. With this purpose, we first write explicitly the Einstein field equations for the interior regular region. We take an electrically charged nonisotropic fluid, which presents spherical symmetry and a de Sitter type equation of state, where the radial pressure [Formula: see text] is equal to the negative of energy density [Formula: see text], [Formula: see text]. Then, two solutions for the Einstein equations are built, a regular interior solution for the region with matter satisfying a de Sitter equation of state, and an external solution for the region outside the matter, that corresponds to the Reissner–Nordström metric. To complete the solution we apply the Darmois–Israel junction conditions with a timelike thin shell at the matching surface. It is assumed that the matching surface is composed by a thin shell of matter, i.e. a surface layer in the form of a perfect fluid obeying a barotropic equation of state, [Formula: see text] and [Formula: see text] being the intrinsic pressure and energy density of the shell, respectively, and [Formula: see text] a constant parameter. We show that there are electrically charged regular black hole solutions and other compact objects for specific choices of [Formula: see text] and of the other parameters of the model. Some properties the objects are investigated.

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Revisiting Relativistic Electrically Charged Polytropic Spheres

Aceña,

Cardin Guntsche,

Gentile de Austria

2024

Annalen der Physik

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The problem of the structure and physical properties of electrically charged static spherically symmetric solutions of the Einstein‐Maxwell system of equations is revisited, where the matter model is a polytropic gas. A relativistic polytrope equation of state (EOS) is considered and the electric charge density is assumed to be proportional to the rest mass density. Families of solutions corresponding to various sets of parameters are constructed and analyzed their stability and compliance with the causality requirement, emphasizing the possibility of obtaining black hole mimickers. Concretely, this study wants to test how much electric charge a given object can hold and how compact it can be. It is concluded that there is a microscopic bound on the charge density to rest mass density ratio coincident with the macroscopic bound regarding the extremal Reissner‐Nordström (ERN) black hole. The macroscopic charge to mass ratio for the object can exceed the corresponding microscopic ratio if the object is non‐extremal. Crucially, the only way to construct a black hole mimicker is by taking a subtle limit in which an electrically counterpoised dust (ECD) solution is attained.

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Compact objects in general relativity: From Buchdahl stars to quasiblack holes

Cited by 11 publications

References 74 publications

All fundamental electrically charged thin shells in general relativity: From star shells to tension shell black holes and regular black holes and beyond

All fundamental electrically charged thin shells in general relativity: From star shells to tension shell black holes and regular black holes and beyond

New regular black hole solutions and other electrically charged compact objects with a de Sitter core and a matter layer

Revisiting Relativistic Electrically Charged Polytropic Spheres

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