Cellular Dynamo in a Rotating Spherical Shell Alexander Getling Lomonosov Moscow State University Moscow, Russia Radostin Simitev, Friedrich Busse University.

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Presentation transcript:

Cellular Dynamo in a Rotating Spherical Shell Alexander Getling Lomonosov Moscow State University Moscow, Russia Radostin Simitev, Friedrich Busse University of Bayreuth, Germany Cellular Dynamo in a Rotating Spherical Shell Alexander Getling Lomonosov Moscow State University Moscow, Russia Radostin Simitev, Friedrich Busse University of Bayreuth, Germany

The problem of solar dynamo: interplay between global and local magnetic fields needs to be included Mean-field electrodynamics → no local fields considered no local fields considered Possible alternative → “deterministic” dynamo with well-defined “deterministic” dynamo with well-defined structural elements in the flow and structural elements in the flow and magnetic field magnetic field

Kinematic model of cellular dynamo (cell = toroidal eddy): A.V. Getling and B.A. Tverskoy, Geomagn. Aeron. 11, 211, 389 (1971)

Convective mechanism of magnetic-field amplification and structuring

This study is based on numerical simulations of cellular magnetoconvection in a rotating spherical shell

The problem Spherical fluid shell Spherical fluid shell Stress-free, electrically insulating boundaries with perfect heat conductivity Stress-free, electrically insulating boundaries with perfect heat conductivity Uniformly distributed internal heat sources Uniformly distributed internal heat sources Boussinesq approximation Boussinesq approximation A small quadratic term is present in the temperature dependence of density A small quadratic term is present in the temperature dependence of density

The geometry of the problem

Static temperature profile

Physical parameters of the problem

The case discussed here Geometrical parameter: η = 0.6 Physical parameters: R i = 3000, R e = − 6000, τ = 10, P = 1, P m =30 Computational parameter: m = 5

Static profiles of temperature and its gradient

Pseudospectral code employed: F.H. Busse, E. Grote, and A. Tilgner, Stud. Geophys. Geod. 42, 211 (1998)

Radial velocity at r = r i d t = 98.73

Azimuthal velocity and meridional streamlines t = 98.73

Radial magnetic field at r = r o d t = 98.73t =

Radial magnetic field at r = r o

Azimuthal magnetic field and meridional field lines t = 95.73t =

Variations in poloidal components H 1 0 and H 2 0 at r = 0.5

Variations in full magnetic energy

Variations in dipolar-field energy axisymm. pol. axisymm. tor. asymm. pol. asymm. tor.

Thank you for your attention