Articles | Volume 11, issue 5/6
Nonlin. Processes Geophys., 11, 619–629, 2004
https://doi.org/10.5194/npg-11-619-2004

Special issue: Advances in space environment turbulence

Nonlin. Processes Geophys., 11, 619–629, 2004
https://doi.org/10.5194/npg-11-619-2004

  03 Dec 2004

03 Dec 2004

Direct numerical simulations of helical dynamo action: MHD and beyond

D. O. Gómez1,* and P. D. Mininni2 D. O. Gómez and P. D. Mininni
  • 1Departamento de Física, Facultad de Ciencias Exactas y Naturales, Universidad de Buenos Aires, Ciudad Universitaria, 1428 Buenos Aires, Argentina
  • 2Advanced Study Program, National Center for Atmospheric Research, P.O. Box 3000, Boulder, Colorado 80307, USA
  • *also at: Instituto de Astronomía y Física del Espacio, CONICET, Ciudad Universitaria, 1428 Buenos Aires, Argentina

Abstract. Magnetohydrodynamic dynamo action is often invoked to explain the existence of magnetic fields in several astronomical objects. In this work, we present direct numerical simulations of MHD helical dynamos, to study the exponential growth and saturation of magnetic fields. Simulations are made within the framework of incompressible flows and using periodic boundary conditions. The statistical properties of the flow are studied, and it is found that its helicity displays strong spatial fluctuations. Regions with large kinetic helicity are also strongly concentrated in space, forming elongated structures. In dynamo simulations using these flows, we found that the growth rate and the saturation level of magnetic energy and magnetic helicity reach an asymptotic value as the Reynolds number is increased. Finally, extensions of the MHD theory to include kinetic effects relevant in astrophysical environments are discussed.