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

scholarly journals Numerical Modelling of Heat and Magnetohydrodynamic Flows in a Finite Cylinder

2002 ◽  
Vol 2 (3) ◽  
pp. 243-259 ◽  
Author(s):  
Andris Buikis ◽  
Harijs Kalis
Keyword(s):  
Finite Difference ◽  
Mhd Flow ◽  
Original Method ◽  
Finite Cylinder ◽  
Symmetric System ◽  
Finite Difference Schemes ◽  
Axially Symmetric ◽  
Mean Values ◽  
Magnetohydrodynamic Flows ◽  
Three Phase

AbstractThe distribution of electromagnetic fields, forces and temperatures induced by a three- phase axially-symmetric system of electric current in a conducting cylinder of finite length has been calculated. An original method was used to calculate the mean values of electromagnetic forces. The magnetohydrodynamic (MHD) flow of viscous incompressible liquid and distribution of temperature are obtained by the finite-difference method, using monotonic finite difference schemes.

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.

MHD FLOW AND HEAT TRANSFER IN A CASSON FLUID OVER A NONLINEARLY STRETCHING SHEET WITH NEWTONIAN HEATING

2018 ◽  
Vol 49 (12) ◽  
pp. 1185-1198 ◽  
Author(s):  
Abid Hussanan ◽  
Mohd Zuki Salleh ◽  
Hamzeh Taha Alkasasbeh ◽  
Ilyas Khan
Keyword(s):  
Heat Transfer ◽  
Stretching Sheet ◽  
Mhd Flow ◽  
Casson Fluid ◽  
Newtonian Heating ◽  
Flow And Heat Transfer ◽  
Nonlinearly Stretching Sheet

HEAT TRANSFER IN NANOFLUID MHD FLOW IN A CHANNEL WITH PERMEABLE WALLS

2017 ◽  
Vol 48 (3) ◽  
pp. 221-238 ◽  
Author(s):  
Mehdi Fakour ◽  
D.D. Ganji ◽  
A. Khalili ◽  
A. Bakhshi
Keyword(s):  
Heat Transfer ◽  
Mhd Flow ◽  
Permeable Walls
Sign in / Sign up

Export Citation Format

Share Document