scholarly journals Kinematic Dynamo by Parity-Antisymmetric Flows

2018 ◽  
pp. 83-95
Author(s):  
Aleksandr Andrievsky ◽  
◽  
Vladislav Zheligovsky ◽  
Roman Chertovskikh ◽  
◽  
...  
Keyword(s):  
Kinematic Dynamo

Effects of conductivity jumps in the envelope of a kinematic dynamo flow

2006 ◽  
Vol 334 (10) ◽  
pp. 593-598 ◽  
Author(s):  
Raphael Laguerre ◽  
Caroline Nore ◽  
Jacques Léorat ◽  
Jean-Luc Guermond
Keyword(s):  
Kinematic Dynamo

scholarly journals Numerical simulations of kinematic dynamo action

2002 ◽  
Vol 397 (2) ◽  
pp. 393-399 ◽  
Author(s):  
V. Archontis ◽  
S. B. F. Dorch ◽  
Å. Nordlund
Keyword(s):  
Numerical Simulations ◽  
Dynamo Action ◽  
Kinematic Dynamo

Kinematic dynamo simulations of von Kármán flows: application to the VKS experiment

2010 ◽  
Vol 74 (2) ◽  
pp. 165-176 ◽  
Author(s):  
A. Pinter ◽  
B. Dubrulle ◽  
F. Daviaud
Keyword(s):  
Kinematic Dynamo ◽  
Von Karman ◽  
Von Kármán

scholarly journals Helioseismic inferences

2009 ◽  
Vol 5 (S264) ◽  
pp. 33-38
Author(s):  
Hiromoto Shibahashi
Keyword(s):  
Solar Activity ◽  
Linear Approximation ◽  
Activity Cycle ◽  
Solar Activity Cycle ◽  
Convective Zone ◽  
Dynamo Model ◽  
Kinematic Dynamo ◽  
Wide Range ◽  
Dynamo Mechanism ◽  
Solar Type

AbstractThe brilliant outcome of some 30 years of helioseismology spreads over a wide range of topics. Some highlights relevant to the cause of the solar activity cycle are listed up. The rotation profile in the solar convective zone is discussed as an important source of the dynamo mechanism. The kinematic dynamo model is described in the linear approximation, and the condition for the solar type dynamo is derived. It is shown that comparison of this condition with the rotation profile determined from helioseismology is useful to identify the possible seats of the dynamo.

Kinematic dynamo problem in a linear velocity field

1984 ◽  
Vol 144 ◽  
pp. 1-11 ◽  
Author(s):  
Ya. B. Zel'Dovich ◽  
A. A. Ruzmaikin ◽  
S. A. Molchanov ◽  
D. D. Sokoloff
Keyword(s):  
Magnetic Field ◽  
Spatial Distribution ◽  
Velocity Field ◽  
Random Matrix ◽  
Magnetic Energy ◽  
Linear Velocity ◽  
Finite Conductivity ◽  
Kinematic Dynamo ◽  
Linear Velocity Field ◽  
The Magnetic Field

A magnetic field is shown to be asymptotically (t → ∞) decaying in a flow of finite conductivity with v = Cr, where C = Cζ(t) is a random matrix. The decay is exponential, and its rate does not depend on the conductivity. However, the magnetic energy increases exponentially owing to growth of the domain occupied by the field. The spatial distribution of the magnetic field is a set of thin ropes and (or) layers.

Transition fields from kinematic dynamo calculations

1996 ◽  
Vol 17 (2) ◽  
pp. 215-218
Author(s):  
Graeme Sarson
Keyword(s):  
Kinematic Dynamo
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