Long-term temporal variations in the areas of sunspot groups

TL;DR

This study extends previous analysis of sunspot group data from 1874-2011, examining long-term and cycle-related variations in the mean maximum sizes of different sunspot group classes and their correlation with solar activity indicators.

Contribution

It introduces an analysis of mean maximum sizes of sunspot groups over long periods and identifies specific cyclic patterns and their potential relation to solar activity phases.

Findings

No significant correlation between mean maximum size and sunspot number.

Approximately 9-year cycle in large and big sunspot groups.

Strong 130+ year cycle in small sunspot group sizes.

Abstract

Recently, we analyzed the combined Greenwich and Solar Optical Observing Network (SOON) sunspot group data during the period 1874-2011 and studied variations in the annual numbers of small, large and big sunspot groups. Here that analysis is extended and studied variations in the mean maximum sizes (the mean values of maximum areas) of the aforementioned three classes of sunspot groups and also their combination. It is found that there is no significant correlation between the mean maximum size of any class of sunspot groups and the International Sunspot Number (Rz), probably due to in a given time interval small sunspot groups/sunspots outnumber the large ones. A pattern of an approximate 9-year period cycle is seen in the variations of the mean maximum sizes of the large and the big sunspot groups during a solar cycle. On long-time scales it is found that there exists a strong 130 or more years cycle in the variation of the mean size of the small sunspot groups, whereas there is a hint on the existence of approximate 44-year cycles in the variations of the mean maximum sizes of the large and the big sunspot groups. During the decline phase of cycle 23, there was a scarcity in the very small sunspot groups (maximum area AM < or = 37 msh), which may be related to the slow growth of sunspot groups during this period. During the minimum between cycles 23 and 24 may be due to the presence of a number of small sunspot groups whose AM > 37 msh was larger than that of whose AM < or = 37 msh, the relatively large size coronal holes were present at low-latitudes and the total solar irradiance was very low.