Latitude Distribution of Sunspots: Analysis Using Sunspot Data and a Dynamo Model

Abstract

In this paper, we explore the evolution of sunspot latitude distribution and explore its relations with the cycle strength. With the progress of the solar cycle, the distributions in two hemispheres from mid-latitudes propagate toward the equator and then ( before the usual solar minimum ) these two distributions touch each other. By visualizing the evolution of the distributions in two hemispheres, we separate the solar cycles by excluding this hemispheric overlap. From these isolated solar cycles in two hemispheres, we generate latitude distributions for each cycle, starting from cycle 8 to cycle 23. We fi nd that the parameters of these distributions, namely the central latitude ( C ) , width ( δ ) , and height ( H ) , evolve with the cycle number, and they show some hemispheric asymmetries. Although the asymmetries in these parameters persist for a few successive cycles, they get corrected within a few cycles, and the new asymmetries appear again. In agreement with the previous study, we fi nd that distribution parameters are correlated with the strengths of the cycles, although these correlations are signi fi cantly different in two hemispheres. The general trend features, i.e., ( i ) stronger cycles that begin sunspot eruptions at relatively higher latitudes, and ( ii ) stronger cycles that have wider bands of sunspot emergence latitudes, are con fi rmed when combining the data from two hemispheres. We explore these features using a fl ux transport dynamo model with stochastic fl uctuations. We fi nd that these features are correctly reproduced in this model. The solar cycle evolution of the distribution center is also in good agreement with observations. Possible explanations of the observed features based on this dynamo model are presented.