New axially symmetric solutions of the Einstein-Maxwell equations

1990 ◽  
Vol 22 (7) ◽  
pp. 799-809 ◽  
Author(s):  
V. S. Manko
Keyword(s):  
Maxwell Equations ◽  
Axially Symmetric

A solution of the stationary axially symmetric Brans-Dicke-Maxwell equations

1981 ◽  
Vol 85 (6-7) ◽  
pp. 316-318
Author(s):  
K.D. Krori ◽  
T. Chaudhury ◽  
R. Bhattacharjee ◽  
B.B. Paul
Keyword(s):  
Maxwell Equations ◽  
Axially Symmetric

Whistler wave propagation in density ducts

1982 ◽  
Vol 27 (2) ◽  
pp. 225-238 ◽  
Author(s):  
V. I. Karpman ◽  
R. N. Kaufman
Keyword(s):  
Wave Propagation ◽  
Maxwell Equations ◽  
Wave Attenuation ◽  
Wave Length ◽  
Whistler Wave ◽  
Analytical Theory ◽  
Ray Theory ◽  
Axially Symmetric ◽  
Symmetric Density ◽  
Attenuation Rate

A theory of whistler wave propagation in axially symmetric density ducts is developed. Both density crests and troughs are considered. The duct width is assumed to be large compared with the parallel wave length. All considerations are based on the Maxwell equations. A number of effects that are not included in the ray theory and (or) the Schrödinger-type equations are elucidated. Among them is whistler detrapping from a density crest at ω < ½ωH. An analytical theory of the detrapping is developed and the corresponding wave attenuation rate in the duct is calculated.

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 &amp; 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.

Sign in / Sign up

Export Citation Format

Share Document