Shape-invariance error for axially symmetric light beams

1998 ◽  
Vol 34 (11) ◽  
pp. 2109-2116 ◽  
Author(s):  
S. Vicalvi ◽  
R. Borghi ◽  
M. Santarsiero ◽  
F. Gori
Keyword(s):  
Axially Symmetric ◽  
Shape Invariance ◽  
Light Beams

Shape invariance characterization of coherent axially symmetric beams

1996 ◽  
Author(s):  
Franco Gori ◽  
Riccardo Borghi ◽  
Massimo Santarsiero ◽  
Silvia Vicalvi
Keyword(s):  
Axially Symmetric ◽  
Shape Invariance

Self-action of Counterpropagating Axially Symmetric Light Beams in a Transparent Cubic-nonlinearity Medium

1991 ◽  
Vol 38 (6) ◽  
pp. 1189-1202 ◽  
Author(s):  
A.A. Afanas'ev ◽  
V.I. Kruglov ◽  
B.A. Samson ◽  
R. Jakyte ◽  
V.M. Volkov
Keyword(s):  
Axially Symmetric ◽  
Cubic Nonlinearity ◽  
Light Beams

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.

Unstable axially symmetric mhd flow between rotating boundaries

2001 ◽  
Vol 7 (2s) ◽  
pp. 19-25
Author(s):  
A.A. Loginov ◽  
◽  
Yu.I. Samoilenko ◽  
V.A. Tkachenko ◽  
◽  
...  
Keyword(s):  
Mhd Flow ◽  
Axially Symmetric
Sign in / Sign up

Export Citation Format

Share Document