Theoretical interpretation of the variability of global solar properties

As the Sun evolves through a magnetic cycle the distribution and amplitude of magnetic regions is altered. Surface phenomena (e.g., sunspots, faculae, and coronal structures) signify clearly the variations, but it is less obvious how the global, interior structure of the Sun responds. Theory suggests that the interior structure may respond directly to the magnetic fields via their associated pressure, and that convective energy transport efficiency will be perturbed. The changes of diameter and luminosity (and thus effective temperature) depend upon details of assumed mechanisms and the position in the interior at which they are applied. The p-mode oscillation frequencies can be perturbed either via changes in the mean structure, or by interaction with distributed magnetic field domains. No definitive variations of diameter, p-mode frequencies, effective temperature, neutrino flux, etc. have yet been shown to exist.