Equatorial symmetry/antisymmetry of stationary axisymmetric electrovac spacetimes: II

Ernst, Frederick J.; Manko, V. S.; Ruiz, E.

doi:10.1088/0264-9381/24/9/003

Cited by 14 publications

(27 citation statements)

References 20 publications

Supporting

Mentioning

Contrasting

Order By: Relevance

“…The above expressions support the physical meaning attributed to the parameters of EMR solutions in the paper [2]. From (27) and (28) follows that the main difference between the two solutions lies in the structure of the electromagnetic moments: in solution I the odd moments Q 2n+1 and H 2n+1 are equal to zero, whereas in solution II are equal to zero the even moments Q 2n and H 2n .…”

Section: The Multipole Moments Basic Limits Stationary Limit Surfacsupporting

confidence: 72%

See 1 more Smart Citation

On the properties of the Ernst–Manko–Ruiz equatorially antisymmetric solutions

Sod–Hoffs

Rodchenko

2007

Class. Quantum Grav.

View full text Add to dashboard Cite

Abstract. Two new equatorially antisymmetric solutions recently published by Ernst et al are studied. For both solutions the full set of metric functions is derived in explicit analytic form and the behavior of the solutions on the symmetry axis is analyzed. It is shown in particular that two counter-rotating equal Kerr-Newman-NUT objects will be in equilibrium when the condition m 2 + ν 2 = q 2 + b 2 is verified, whereas two counter-rotating equal masses endowed with arbitrary magnetic and electric dipole moments cannot reach equilibrium under any choice of the parameters, so that a massless strut between them will always be present.

show abstract

Section: The Multipole Moments Basic Limits Stationary Limit Surfacsupporting

confidence: 72%

“…It is worthwhile mentioning that an arbitrary additive constant in the expression of ω in (16) was chosen in such a way that the constant ω 0 in the definition of equatorially antisymmetric spacetimes [2] were equal to zero, i.e., ω(ρ, z) = −ω(ρ, −z) automatically.…”

Section: The Ernst Potentials and Metric Functions Of Emr Solutionsmentioning

confidence: 99%

On the properties of the Ernst–Manko–Ruiz equatorially antisymmetric solutions

Sod–Hoffs

Rodchenko

2007

Class. Quantum Grav.

View full text Add to dashboard Cite

show abstract

“…Having in mind the idea of improving the presentation of the vacuum MMR metric, recently we have carefully revised our earlier work on the extended two-soliton solutions, exploring in particular various ways of writing the metric function ω of which we have finally chosen the one that looked to us more attractive than the others. However, before the presentation of the metric functions of the MMR solution, below we first write down the form of the Ernst potential E of the latter solution [1,31]:…”

Section: The Mmr 4-parameter Vacuum Solutionmentioning

confidence: 99%

Exterior field of slowly and rapidly rotating neutron stars: Rehabilitating spacetime metrics involving hyperextreme objects

Manko

Ruiz

2016

Phys. Rev. D

View full text Add to dashboard Cite

The 4-parameter exact solution presumably describing the exterior gravitational field of a generic neutron star is presented in a concise explicit form defined by only three potentials. In the equatorial plane, the metric functions of the solution are found to be given by particularly simple expressions that make them very suitable for the use in concrete applications. Following Pappas and Apostolatos, we perform a comparison of the multipole structure of the solution with the multipole moments of the known physically realistic Berti-Stergioulas numerical models of neutron stars to argue that the hyperextreme sectors of the solution are not less (but possibly even more) important for the correct description of rapidly rotating neutron stars than the subextreme sector involving exclusively the black-hole constituents. We have also worked out in explicit form an exact analog of the well-known Hartle-Thorne approximate metric.

show abstract

“…[9] for an equatorially antisymmetric spacetime [14] with both electric and magnetic dipole moments:…”

Section: The Five-parameter Asymptotically Flat Emr Solution In σmentioning

confidence: 99%

Stationary black diholes

Manko¹,

Rabadán²,

Sanabria-Gómez³

2014

Phys. Rev. D

View full text Add to dashboard Cite

In this paper we present and analyze the simplest physically meaningful model for stationary black diholes - a binary configuration of counter-rotating Kerr-Newman black holes endowed with opposite electric charges - elaborated in a physical parametrization on the basis of one of the Ernst-Manko-Ruiz equatorially antisymmetric solutions of the Einstein-Maxwell equations. The model saturates the Gabach-Clement inequality for interacting black holes with struts, and in the absence of rotation it reduces to the Emparan-Teo electric dihole solution. The physical characteristics of each dihole constituent satisfy identically the well-known Smarr's mass formula.Comment: 19 pages, 3 figures; small changes taking into account referee's suggestion

show abstract

Equatorial symmetry/antisymmetry of stationary axisymmetric electrovac spacetimes: II

Cited by 14 publications

References 20 publications

On the properties of the Ernst–Manko–Ruiz equatorially antisymmetric solutions

On the properties of the Ernst–Manko–Ruiz equatorially antisymmetric solutions

Exterior field of slowly and rapidly rotating neutron stars: Rehabilitating spacetime metrics involving hyperextreme objects

Stationary black diholes

Contact Info

Product

Resources

About