Angular dependence of the facular-sunspot coverage relation as derived by MDI magnetograms

TL;DR

This study investigates how the relationship between facular and sunspot coverage varies across the solar disk and over time, using MDI magnetograms, revealing dependencies on position, flux, and solar cycle phase.

Contribution

It provides a detailed analysis of the angular dependence of facular-sunspot relations, incorporating magnetic flux and cycle phase, which enhances understanding for solar irradiance models.

Findings

Quadratic fit best for daily data; linear for 6-month averages.

Coefficients depend on disk position and magnetic flux.

Asymmetries observed between solar cycle phases near disk center.

Abstract

Previous studies have shown that the variation over the solar magnetic activity cycle of the area of facular/network features identified on broad band and narrow band imagery is positively correlated with the sunspot area and number, the relation between the area coverages being described as either linear or quadratic. On the other hand, the temporal variation of the spatial distributions of faculae, network and sunspots follows patterns that are less obviously correlated, so that we expect the relation that describes variation of the area coverage of different types of magnetic features to vary with the position over the disk. In this work we employ MDI full-disk magnetograms acquired during Cycle 23 and at the beginning of Cycle 24 to investigate the relation between the coverage of magnetic elements characterized by different amounts of magnetic flux and located at different angular distances from disk center with the sunspot number. In agreement with some previous studies we find that daily data are best described by a quadratic function while data averaged over 6-months are best described by a linear function. In both cases the coefficients of the fits show large dependence on the position over the disk and the magnetic flux. We also find that toward disk center 6-months averaged data show asymmetries between the ascending and the descending phase. Implications for solar irradiance modeling are discussed.