3,247 research outputs found
Newman Tamburino solutions with an aligned Maxwell field
No full textWe prove that there exists no aligned Einstein Maxwell generalization of the spherical class of Newman Tamburino solutions. The presence of an aligned Maxwell field automatically leads to the cylindrical class
Analytic study of the Maxwell electromagnetic invariant in spinning and charged Kerr-Newman black-hole spacetimes
No full textThe Maxwell invariant plays a fundamental role in the mathematical
description of electromagnetic fields in charged spacetimes. We present a
detailed {\it analytical} study of the physical and mathematical properties of
the Maxwell electromagnetic invariant
which characterizes the Kerr-Newman black-hole spacetime. It is proved that,
for all Kerr-Newman black-hole spacetimes, the spin and charge dependent
minimum value of the Maxwell electromagnetic invariant is attained on the
equator of the black-hole surface. Interestingly, we reveal the physically
important fact that Kerr-Newman spacetimes are characterized by two critical
values of the dimensionless rotation parameter , and , which mark the boundaries between three qualitatively
different spatial functional behaviors of the Maxwell electromagnetic
invariant: (i) Kerr-Newman black holes in the slow-rotation regime are characterized by negative definite Maxwell
electromagnetic invariants that increase monotonically towards spatial
infinity, (ii) for black holes in the intermediate spin regime , the positive
global maximum of the Kerr-Newman Maxwell electromagnetic invariant is located
at the black-hole poles, and (iii) Kerr-Newman black holes in the
super-critical regime are characterized
by a non-monotonic spatial behavior of the Maxwell electromagnetic invariant
along the black-hole horizon with a spin and charge dependent global maximum
whose polar angular location is characterized by the dimensionless functional
relation .Comment: 20 page
Analytic study of the Maxwell electromagnetic invariant in spinning and charged Kerr-Newman black-hole spacetimes
No full textAbstract The Maxwell invariant plays a fundamental role in the mathematical description of electromagnetic fields in charged spacetimes. In particular, it has recently been proved that spatially regular scalar fields which are non-minimally coupled to the Maxwell electromagnetic invariant can be supported by spinning and charged Kerr-Newman black holes. Motivated by this physically intriguing property of asymptotically flat black holes in composed Einstein-Maxwell-scalar field theories, we present a detailed analytical study of the physical and mathematical properties of the Maxwell electromagnetic invariant F KN r θ M a Q which characterizes the Kerr-Newman black-hole spacetime [here {r, θ} are respectively the radial and polar coordinates of the curved spacetime and {M, J = M a, Q} are respectively the mass, angular momentum, and electric charge parameters of the black hole]. It is proved that, for all Kerr-Newman black-hole spacetimes, the spin and charge dependent minimum value of the Maxwell electromagnetic invariant is attained on the equator of the black-hole surface. Interestingly, we reveal the physically important fact that Kerr-Newman spacetimes are characterized by two critical values of the dimensionless rotation parameter a ̂ ≡ a / r + [here r + (M, a, Q) is the black-hole horizon radius], a ̂ crit − = 3 − 2 2 and a ̂ crit + = 5 − 2 5 , which mark the boundaries between three qualitatively different spatial functional behaviors of the Maxwell electromagnetic invariant: (i) Kerr-Newman black holes in the slow-rotation a ̂ < a ̂ crit − regime are characterized by negative definite Maxwell electromagnetic invariants that increase monotonically towards spatial infinity, (ii) for black holes in the intermediate spin regime a ̂ crit − ≤ a ̂ ≤ a ̂ crit + , the positive global maximum of the Kerr-Newman Maxwell electromagnetic invariant is located at the black-hole poles, and (iii) Kerr-Newman black holes in the super-critical regime a ̂ < a ̂ crit + are characterized by a non-monotonic spatial behavior of the Maxwell electromagnetic invariant F KN r = r + θ M a Q along the black-hole horizon with a spin and charge dependent global maximum whose polar angular location is characterized by the dimensionless functional relation a ̂ 2 · (cos2 θ)max = 5 – 2 5
The Kerr-Newman metric: A review
No full textThe Kerr-Newman metric describes a very special rotating, charged mass and is the most general of the asymptotically flat stationary ‘black hole’ solutions to the Einstein-Maxwell equations of general relativity. We review the derivation of this metric from the Reissner-Nordström solution by means of a complex transformation algorithm and provide a brief overview of its basic geometric properties. We also include some discussion of interpretive issues, related metrics, and higher-dimensional analogues
Complete integration of the aligned Newman Tamburino Maxwell solutions
No full textWe investigate the cylindrical class of Newman Tamburino equations in the presence of an aligned Maxwell field. After obtaining a complete integration of the field equations we look at the possible vacuum limits and we examine the symmetries of the general solution
Tuttiett, Mary Gleed [pseud. Maxwell Gray] (1846–1923), novelist
No full textBiographical entry of popular female author Maxwell Gray
Corrections to Kerr-Newman black hole from noncommutative Einstein-Maxwell equation
No full textIn this letter we introduce the noncommutative geometry into the standard Einstein-Hilbert-Maxwell action via the ∂t∧∂φ Drinfeld twist and solve the equation of motion pertubatively in the expansion of the noncommutative parameter a. The equation of motion, the NC Einstein-Maxwell equation, turns out to be effectively a problem in nonlinear electrodynamics where the energy-momentum tensor Tμν obtains correction terms with three Faraday tensors Fμν. A solution with nonzero a1 terms turns out to be the Kerr-Newman black hole modified with nonzero gtθ,grφ,gtr and gφθ components proportional to a, while the electromagnetic potential is the Seiberg-Witten expanded Kerr-Newman potential which introduces a nonzero Aθ term proportional to a
Interacting Kerr-Newman electromagnetic fields
No full textIn this paper, we study some of the properties of the →0 limit of the Kerr-Newman solution of Einstein-Maxwell equations. Carter noted the near equality between the gyromagnetic ratio, or g-factor, of the Kerr-Newman solution and of the electron. This observation is a consequence of the multipole structure of the Kerr-Newman field. We discuss additional coincidences between the Kerr-Newman multipole structure and the properties of the electron. In contrast to the Coulomb field, this spinning Maxwell field has a finite Lagrangian. Moreover, by evaluating the Lagrangian for the superposition of two such Kerr-Newman electromagnetic fields on a flat background, we are able to find their interaction potential. This yields a correction to the Coulomb interaction due to the spin of the field.</p
The Euclidean quantisation of Kerr-Newman-de Sitter black holes
No full textWe study the family of Einstein-Maxwell instantons associated with the Kerr-Newman metrics with a positive cosmological constant. This leads to a quantisation condition on the masses, charges, and angular momentum parameters of the resulting Euclidean solutions.© The Author(s) 201
Interacting Kerr-Newman Electromagnetic Fields
No full textIn this paper, we study some of the properties of the limit of the
Kerr-Newman solution of Einstein-Maxwell equations. Noting Carter's observation
of the near equality between the gyromagnetic ratio in the Kerr-Newman
solution and that of the electron, we discuss additional such coincidences
relating to the Kerr-Newman multipoles and properties of the electron. In
contrast to the Coulomb field, this spinning Maxwell field has a finite
Lagrangian. Moreover, by evaluating the Lagrangian for the superposition of two
such Kerr-Newman electromagnetic fields on a flat background, we are able to
find their interaction potential. This yields a correction to the Coulomb
interaction due to the spin of the field.Comment: 30 pages, 11 figures, 3 table
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