Weakly dissipative plasma equilibria in Kerr geometry

2004 ◽  
Vol 11 (1) ◽  
pp. 278-285
Author(s):  
Klaus Elsässer ◽  
Yauhen Kot
Keyword(s):  
Kerr Geometry ◽  
Plasma Equilibria

On embeddings of the Kerr geometry

1981 ◽  
Vol 59 (5) ◽  
pp. 688-692 ◽  
Author(s):  
Nigel A. Sharp
Keyword(s):  
Black Hole ◽  
Event Horizon ◽  
Equatorial Plane ◽  
Kerr Metric ◽  
Intrinsic Structure ◽  
Kerr Geometry ◽  
Rotating Black Hole ◽  
Isometric Embeddings

The use of isometric embeddings of curved geometries reveals their intrinsic structure in a way that is readily appreciated. This is done for 3 two-surfaces sliced from the Kerr metric which describes a rotating black hole: the equatorial plane, the event horizon, and the ergosurface.

A class of new perturbation equations for the Kerr geometry

1982 ◽  
Vol 89 (2) ◽  
pp. 68-70 ◽  
Author(s):  
Misao Sasaki ◽  
Takashi Nakamura
Keyword(s):  
Kerr Geometry ◽  
New Perturbation ◽  
Perturbation Equations

Reflection of a Gaussian beam from a magnetized medium in the polar Kerr geometry

2015 ◽  
Vol 118 (2) ◽  
pp. 310-316
Author(s):  
I. V. Zlodeev ◽  
Yu. F. Nasedkina ◽  
D. I. Sementsov
Keyword(s):  
Gaussian Beam ◽  
Kerr Geometry

scholarly journals Complete set of quasi-conserved quantities for spinning particles around Kerr

2022 ◽  
Vol 12 (1) ◽  
Author(s):  
Geoffrey Compère ◽  
Adrien Druart
Keyword(s):  
Linear Order ◽  
Conserved Quantities ◽  
Killing Tensor ◽  
Kerr Geometry ◽  
Spinning Particles ◽  
Kerr Spacetime ◽  
Killing Tensors ◽  
Mixed Symmetry ◽  
Constants Of Motion ◽  
Complete Set

We revisit the conserved quantities of the Mathisson-Papapetrou-Tulczyjew equations describing the motion of spinning particles on a fixed background. Assuming Ricci-flatness and the existence of a Killing-Yano tensor, we demonstrate that besides the two non-trivial quasi-conserved quantities, i.e. conserved at linear order in the spin, found by Rüdiger, non-trivial quasi-conserved quantities are in one-to-one correspondence with non-trivial mixed-symmetry Killing tensors. We prove that no such stationary and axisymmetric mixed-symmetry Killing tensor exists on the Kerr geometry. We discuss the implications for the motion of spinning particles on Kerr spacetime where the quasi-constants of motion are shown not to be in complete involution.

scholarly journals Test Particle Calculation of Plasma Equilibria

2021 ◽  
Vol 31 (1) ◽  
pp. 100010
Author(s):  
Jonathan Sullivan-Wood ◽  
Daniel Holland
Keyword(s):  
Test Particle ◽  
Plasma Equilibria

scholarly journals Quasi-spherical light cones of the Kerr geometry

1998 ◽  
Vol 15 (8) ◽  
pp. 2289-2301 ◽  
Author(s):  
Frans Pretorius ◽  
Werner Israel
Keyword(s):  
Kerr Geometry

Plasma equilibria in dipolar magnetic configurations

2000 ◽  
Vol 7 (5) ◽  
pp. 1831-1838 ◽  
Author(s):  
S. I. Krasheninnikov ◽  
Peter J. Catto ◽  
R. D. Hazeltine
Keyword(s):  
Plasma Equilibria

Motional Stark effect plasma equilibria during LHCD experiments on PBX-M

1994 ◽  
Author(s):  
F. Paoletti ◽  
S. Batha ◽  
S. Bernabei ◽  
H. Fishman ◽  
R. Hatcher ◽  
...  
Keyword(s):  
Stark Effect ◽  
Motional Stark Effect ◽  
Plasma Equilibria

Safety Factor for the New Exact Plasma Equilibria

2019 ◽  
Vol 74 (2) ◽  
pp. 163-181 ◽  
Author(s):  
Oleg Bogoyavlenskij
Keyword(s):  
Magnetic Field ◽  
Safety Factor ◽  
Axial Symmetry ◽  
Beltrami Equation ◽  
Exact Formula ◽  
Magnetic Star ◽  
Plasma Velocity ◽  
Plasma Equilibria ◽  
Magnetic Rings ◽  
The Magnetic Field

AbstractAn exact formula for the limit of the safety factor q at a magnetic axis is derived for the general up-down asymmetric plasma equilibria possessing axial symmetry, generalizing Bellan’s formula for the up-down symmetric ones. New exact axisymmetric plasma equilibria depending on arbitrary parameters α, ξ, bkn, zkn, where k = 1, ⋯, M, n = 1⋯, N, are constructed (α ≠ 0 is a scaling parameter), which are up-down asymmetric in general. The equilibria are not force-free if ξ ≠ 0 and satisfy Beltrami equation if ξ = 0. For some values of ξ the magnetic field and electric current fluxes have isolated invariant toroidal magnetic rings, for another ξ they have invariant spheroids (blobs) and for some values of ξ both invariant toroidal rings and spheroids (blobs). A generalization of the Chandrasekhar – Fermi – Prendergast magnetostatic model of a magnetic star is presented where plasma velocity V(x) is non-zero.

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