Exact axially symmetric stationary solutions of the Kaluza-Klein-Jordan-Thiry theory

1987 ◽  
Vol 36 (12) ◽  
pp. 3674-3683 ◽  
Author(s):  
William Bruckman
Keyword(s):  
Stationary Solutions ◽  
Axially Symmetric ◽  
Kaluza Klein

GENERALIZED BELINSKY–RUFFINI GEOMETRY

1991 ◽  
Vol 06 (24) ◽  
pp. 2189-2195
Author(s):  
AMIR LEVINSON ◽  
AHARON DAVIDSON
Keyword(s):  
Electric Charge ◽  
Magnetic Moment ◽  
Extra Dimension ◽  
Space Time ◽  
Einstein Equations ◽  
Axially Symmetric ◽  
Relativistic Limit ◽  
Kaluza Klein

Stationary, axially symmetric solutions of Einstein equations in a free 5-dimensional Kaluza–Klein space-time are derived. The electric charge and magnetic moment are generated by a fictitious boost involving the extra dimension. The associated gyromagnetic factor tends to unity at the ultra-relativistic limit. The solution derived interpolates between the Kerr and the Belinsky–Ruffini solutions.

scholarly journals Nonassociative black ellipsoids distorted by R-fluxes and four dimensional thin locally anisotropic accretion disks

2021 ◽  
Vol 81 (12) ◽  
Author(s):  
Laurenţiu Bubuianu ◽  
Sergiu I. Vacaru ◽  
Elşen Veli Veliev
Keyword(s):  
Accretion Disks ◽  
Ricci Tensor ◽  
Stationary Solutions ◽  
Star Products ◽  
Axially Symmetric ◽  
Deformation Method ◽  
Parametric Solutions ◽  
Symmetric Metrics ◽  
Cosmological Constants ◽  
Tangent Bundles

AbstractWe construct nonassociative quasi-stationary solutions describing deformations of Schwarzschild black holes, BHs, to ellipsoid configurations, which can be black ellipsoids, BEs, and/or BHs with ellipsoidal accretion disks. Such solutions are defined by generic off-diagonal symmetric metrics and nonsymmetric components of metrics (which are zero on base four dimensional, 4-d, Lorentz manifold spacetimes but nontrivial in respective 8-d total (co) tangent bundles). Distorted nonassociative BH and BE solutions are found for effective real sources with terms proportional to $$\hbar \kappa $$ ħ κ (for respective Planck and string constants). These sources and related effective nontrivial cosmological constants are determined by nonlinear symmetries and deformations of the Ricci tensor by nonholonomic star products encoding R-flux contributions from string theory. To generate various classes of (non) associative /commutative distorted solutions we generalize and apply the anholonomic frame and connection deformation method for constructing exact and parametric solutions in modified gravity and/or general relativity theories. We study properties of locally anisotropic relativistic, optically thick, could and thin accretion disks around nonassociative distorted BHs, or BEs, when the effects due to the rotation are negligible. Such configurations describe angular anisotropic deformations of axially symmetric astrophysical models when the nonassociative distortions are related to the outer parts of the accretion disks.

Harmonic maps and magnetostatic, axially symmetric solutions of the Kaluza-Klein theory

1986 ◽  
Vol 93 (1) ◽  
pp. 102-112 ◽  
Author(s):  
T. Dereli ◽  
A. Eriş ◽  
A. Karasu
Keyword(s):  
Harmonic Maps ◽  
Axially Symmetric ◽  
Klein Theory ◽  
Kaluza Klein

NON-SINGULAR GLOBAL COSMIC STRINGS

2005 ◽  
Vol 20 (11) ◽  
pp. 2374-2379
Author(s):  
Y. VERBIN ◽  
A. L. LARSEN
Keyword(s):  
Scalar Field ◽  
Cosmic Strings ◽  
Weak Field ◽  
Stationary Solutions ◽  
Linear Sigma Model ◽  
Complex Scalar ◽  
Potential Term ◽  
Weak Field Limit ◽  
Complex Scalar Field ◽  
Kaluza Klein

Non-singular global cosmic strings are found in a non-linear sigma model with a potential term for a self-gravitating complex scalar field. Stationary solutions with angular momentum and possibly linear momentum are obtained by assuming an oscillatory dependence of the scalar field on t, φ and z. This dependence has an effect similar to gauging the global U(1) symmetry of the model, which is actually a Kaluza-Klein reduction from four to three spacetime dimensions. The method of analysis can be regarded as an extension of the gravito-electromagnetism formalism beyond the weak field limit.

scholarly journals Charged fermions tunneling from stationary axially symmetric black holes with generalized uncertainty principle

2019 ◽  
Vol 34 (23) ◽  
pp. 1950184 ◽  
Author(s):  
Muhammad Rizwan ◽  
Muhammad Zubair Ali ◽  
Ali Övgün
Keyword(s):  
Black Holes ◽  
Black Hole ◽  
Uncertainty Principle ◽  
Emission Rate ◽  
Generalized Uncertainty Principle ◽  
Axially Symmetric ◽  
Black String ◽  
Fermions Tunneling ◽  
Newman Black Hole ◽  
Kaluza Klein

In this paper, we study the tunneling of charged fermions from the stationary axially symmetric black holes using the generalized uncertainty principle (GUP) via Wentzel, Kramers, and Brillouin (WKB) method. The emission rate of the charged fermions and corresponding modified Hawking temperature of Kerr–Newman black hole, Einstein–Maxwell-dilaton-axion (EMDA) black hole, Kaluza–Klein dilaton black hole, and then, charged rotating black string are obtained and we show that the corrected thermal spectrum is not purely thermal because of the minimal scale length which cause the black hole’s remnant.

Solar Internal Rotation and Dynamo Waves: A Two-Dimensional Asymptotic Solution in the Convection Zone

2000 ◽  
Vol 179 ◽  
pp. 379-380
Author(s):  
Gaetano Belvedere ◽  
Kirill Kuzanyan ◽  
Dmitry Sokoloff
Keyword(s):  
Magnetic Field ◽  
Asymptotic Solution ◽  
Internal Rotation ◽  
Convection Zone ◽  
General Idea ◽  
Dynamo Model ◽  
Axially Symmetric ◽  
Dynamo Action ◽  
Regeneration Rate ◽  
Dynamo Waves

Extended abstractHere we outline how asymptotic models may contribute to the investigation of mean field dynamos applied to the solar convective zone. We calculate here a spatial 2-D structure of the mean magnetic field, adopting real profiles of the solar internal rotation (the Ω-effect) and an extended prescription of the turbulent α-effect. In our model assumptions we do not prescribe any meridional flow that might seriously affect the resulting generated magnetic fields. We do not assume apriori any region or layer as a preferred site for the dynamo action (such as the overshoot zone), but the location of the α- and Ω-effects results in the propagation of dynamo waves deep in the convection zone. We consider an axially symmetric magnetic field dynamo model in a differentially rotating spherical shell. The main assumption, when using asymptotic WKB methods, is that the absolute value of the dynamo number (regeneration rate) |D| is large, i.e., the spatial scale of the solution is small. Following the general idea of an asymptotic solution for dynamo waves (e.g., Kuzanyan & Sokoloff 1995), we search for a solution in the form of a power series with respect to the small parameter |D|–1/3(short wavelength scale). This solution is of the order of magnitude of exp(i|D|1/3S), where S is a scalar function of position.

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