scholarly journals Inverse transfer of magnetic helicity in direct numerical simulations of compressible isothermal turbulence: helical transfers

2021 ◽  
Vol 921 ◽  
Author(s):  
Jean-Mathieu Teissier ◽  
Wolf-Christian Müller
Keyword(s):  
Numerical Simulations ◽  
Direct Numerical Simulations ◽  
Magnetic Helicity

Abstract

scholarly journals The Solar Dynamo: Old, Recent, and New Problems

2001 ◽  
Vol 203 ◽  
pp. 144-151
Author(s):  
A. Brandenburg
Keyword(s):  
Numerical Simulations ◽  
Mean Field ◽  
Direct Numerical Simulations ◽  
Solar Dynamo ◽  
Magnetic Helicity ◽  
Current Status ◽  
Dynamo Theory ◽  
Inverse Cascade ◽  
Mean Field Dynamo ◽  
Stellar Dynamo

A number of problems of solar and stellar dynamo theory are briefly reviewed and the current status of possible solutions is discussed. Results of direct numerical simulations are described in view of mean-field dynamo theory and the relation between the α-effect and the inverse cascade of magnetic helicity is highlighted. The possibility of ‘catastrophic’ quenching of the α-effect is explained in terms of the constraint placed by the conservation of magnetic helicity.

scholarly journals Magnetic helicity fluxes and their effect on stellar dynamos

2011 ◽  
Vol 7 (S286) ◽  
pp. 49-53
Author(s):  
Simon Candelaresi ◽  
Axel Brandenburg
Keyword(s):  
Numerical Simulations ◽  
Mean Field ◽  
Reynolds Numbers ◽  
Direct Numerical Simulations ◽  
Critical Values ◽  
Magnetic Helicity ◽  
Dynamic Quenching ◽  
Dynamo Action ◽  
One Dimensional ◽  
Field Formalism

AbstractMagnetic helicity fluxes in turbulently driven α2 dynamos are studied to demonstrate their ability to alleviate catastrophic quenching. A one-dimensional mean-field formalism is used to achieve magnetic Reynolds numbers of the order of 105. We study both diffusive magnetic helicity fluxes through the mid-plane as well as those resulting from the recently proposed alternate dynamic quenching formalism. By adding shear we make a parameter scan for the critical values of the shear and forcing parameters for which dynamo action occurs. For this αΩ dynamo we find that the preferred mode is antisymmetric about the mid-plane. This is also verified in 3-D direct numerical simulations.

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