Towards better Constrained Kinematic Dynamo Models: Turbulent Diffusivity and Diffusivity Quenching

Details Towards better Constrained Kinematic Dynamo Models: Turbulent Diffusivity and Diffusivity Quenching Towards better Constrained Kinematic Dynamo Models: Turbulent Diffusivity and Diffusivity Quenching

May 2010

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2010aas...21640116m&link_type=abstract

American Astronomical Society, AAS Meeting #216, #401.16

Astronomy and Astrophysics

Astronomy

Scientific paper

The turbulent magnetic diffusivity in the Solar Convection Zone (SCZ) is one of the most poorly constrained ingredients of mean-field dynamo models. This lack of constrain has previously led to controversy regarding which set of parameters is more appropriate (yielding better solar like solutions) and the generation of radically different cycle predictions. Furthermore, due to the relative freedom in the different parameters associated with it, more often than not it is used to finely tune the dynamo solutions. As of now, the dynamo community seems to have settled on double step diffusivity profiles characterized by low values of diffusivity inside most of the convection zone; notwithstanding that these values of diffusivity are not consistent with theoretical considerations based on mixing-length theory, which suggest much higher values of turbulent diffusivity. To make matters worse, standard kinematic dynamo simulations cannot yield sustainable magnetic cycles using theoretical estimates. Here we study how magnetic diffusivity quenching can provide a physically meaningful way out of this discrepancy and whether standard diffusivity profiles are truly a representation of a physical process. This work is funded by NASA Living With a Star grant NNG05GE47G.

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