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On the photosphere. The problem is that the information about the boundary fields is so poor that it is impossible to produce a plausible solution to the foregoing equation. Raadu and Nakagawa1 have succeeded in constructing model force-free fields for isolated sunspots and bipolar pairs of sunspots. The fieldlines they compute above the model spots do resemble H fibril structure typical of such spots. Another approach to the analysis of the observations was developed by Schmidt . He pointed out that observations of the line-of-sight component of the fields at or near disk center could be identified with an array of fictitious monopoles in the photosphere: a (rf) = Hn (r')/27r (3) where Hn (rf) is the observed normal component of the photospheric field.

1965. Sunspots, Wiley, New York, p. 68. Sheeley, N. , 1971. "The Time Dependence of Magnetic, Velocity and Intensity Fields in the Solar Atmosphere," Solar Magnetic Fields, edited by R. Howard, Reidel, Dordrecht, p. 310. , 1965. "Short Note on the Connection Between the Facular Network and Sunspots," Stellar and Solar Magnetic Fields, edited by R. Lust, North-Holland, Amsterdam, p. 192. Q Severny, A. , 1960. "An Investigation of Magnetic Fields Connected with Solar Flares," Bulletin of the Crimean Astrophysical Observatory, Vol.

Comparison of data for solar cycle 19 (maximum, 1958) and solar cycle 20 (maximum, 1968) illustrates the order of difference which can occur in successive cycles. Smoothed monthly means of sunspot number for the present cycle have reached a maximum of only ~110, whereas in cycle 19 the corresponding value was as high as 200 (Fig. 2). Major flare activity has shown an even greater diminution in the current cycle. Solar cycle 20 is ORGANIZATION OF SOLAR ACTIVITY SMOOTHED SUNSPOT NUMBER 200r CYCLE 21 19 150 100 CYCLE 20 50 0L Fig.

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