Evolution of polar coronal holes and sunspots during cycles 21 and 22

Details Evolution of polar coronal holes and sunspots during cycles 21 and 22 Evolution of polar coronal holes and sunspots during cycles 21 and 22

Oct 1994

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1994soph..154..377b&link_type=abstract

Solar Physics (ISSN 0038-0938), vol. 154, no. 2, p. 377-384

Physics

12

Coronal Holes, Magnetic Poles, Solar Cycles, Statistical Correlation, Sunspots, Field Strength, Prediction Analysis Techniques, Solar Magnetic Field, Stellar Models

Scientific paper

A very good correlation between the evolution of polar coronal hole size and sunspot number half a solar cycle later was found by Bravo and Otaola for solar cycle 21. In this paper we use a more complete set of data to reanalyse the relationship for solar cycle 21 and investigate the same relationship for solar cycle 22. We find that the complete set of data for cycle 21 yields a slightly different time shift for the best correlation between sunspots and holes and that the time shift for cycle 22 is different from that of cycle 21. However, because of limited availability of data of cycle 22, we consider it necessary to wait until the end of this cycle in order to decide if the difference is statisically significant or not. We also found that the time between successive peaks of smoothed polar hole area and smoothed sunspot number is the same in both cycles. This may provide a useful tool for the forecasting of future sunspot maxima. The constant of proportionality between polar coronal hole area and sunspot number can be seen to be different in both cycles. We discuss this difference and interpret it in terms of a different magnitude of the polar field strength in the two cycles.

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