Title: Photospheric Energy Budgets
Author: James Armstrong
Affil: University Of Hawaii
Email: armstron@ifa.hawaii.edu
Authors: Jeff Kuhn
Affils: University of Hawaii
Abstract: The solar cycle problem is one that has been observed for hundreds of years, yet the mechanisms that are responsible for driving this 22 year cycle are not yet well understood. Further, we do not understand how the observable changes in the surface of the sun affect the solar irradiance. Several approaches have been developed to relate observed features in CaK and in the local magnetic field, however these are purely phenomenological models. While they do have some predictive power, they do not address what is actually driving the observed variations in the irradiance. They tend to assume that the relationship between the excess energy emitted and the area of a facular region is linear. However, it is much more complex, and radiated energy is, at least in part, redistributed by surface features. The redistribution can occur in two ways: 1) The flux emitted is anisotropic, and 2) Excess entropy convecting upward can diffuse into the surrounding region. Sunspots represent an energy deficit in these models, however, our analysis shows that at least 40deficit can be accounted for by the region surrounding a sunspot. Additionally we will discuss the energy budget of facular regions, and provide links to the underlying physical process.