Does the sun have a memory?

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Solar Activity: Dynamo Theory, Solar Convective Zone: Solar Activity Cycles

Scientific paper

The authors study the effect of stochastic fluctuations in α using a simple axisymmetric mean field dynamo model. There are two main features: Firstly, the excitation of higher eigenmodes of the dynamo equation, providing a possible explanation of asymmetries between the two hemispheres and, close to the equator, the formation of small regions of the "wrong" polarity. Secondly, a correlation between fluctuations in phase and amplitude of the dipole field. Phase and amplitude are not locked onto one another, i.e. the dynamo has no "memory". The authors use the phase-amplitude correlation to compare the model with sunspot data, where a similar correlation is observed. This provides a rough estimate of the required strength of the α-fluctuations. It is found that α, defined as an azimuthal average, has fluctuations of the order δα/α0 ≍ 3 at mid latitudes.

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