A clearly evident large-scalc pattern in the interplanetary magnetic field during 1964 is used to search for a similar large-scale pattern in thc selar magnetic field. It is found that such a pattern did exist in the photospheric ticld observations on both sides of the equator over a range of at least 40:N to 35:S. The pattern is basically similar at all these latitudes, and differs from that to be expected from solar differential rotation in three important respects. It is found that the solar magnetic pattern changed at all latitudes investigated within an interval of a few solar rotations.
A dominant feature of the large-scale organization of the interplanetary magnetic field is the sector structure, in which the field has a pronounced tendency to be directed predominantly toward the sun or away from the sun within a sizable sector. The evolution with. time over an interval, of several years of the interplanetary field sector structure is shown in. Figure I. In the present investigation attention is directed toward the interval o1" about 1 year, from. December 1963 to December 1964. At the beginning of this interval the interplanetary field was observed by the satellite IMP-1 (WH_cox and N~ss, 1965), and at the end of this interval the field was observed by IMP-2 (FAn, fIELD and N~ss, 1967) and by Mariner 4 (CoI.f:a.IAy et aL, 1967). As can be seen in Figure 1, the interplanetary sector pattern observed by 1MP-I at the beginning of this interval was very similar to the sector pattern observed by 1MP-2 and Mariner 4 at the end of the interwfi. We assume that the sector pattern did not change appreciably during this interval of I year, and make the interpolation indicated in Figure I. Some evidence supporting this interpolation is as follows. WILCOX and NEss (1965) have shown that gcomagnetic activity tends to be large in the preceding (in the sense of solar rotation) portion of a sector. I n. Figure I we see, c.g., that at the time observed by IMP-I geomagnetic activity is large in. the preceding portion of each individual sector and tends to trail offin the following portions of the sectors. We also can observe vertical columns of enhanced geomagnetic activity extending in a continuous manner from the time observed by IMP-I to the time observed by IMP-2 and Mariner 4. The presence of these vertical columns of geomagnetic activity is strong evidence in support of the interpolated sector pattern. Wlucox and N~ss (1965) have further demonstrated that the interplanetary sector pattern has a considerable influence on the intensity of galactic cosm.ic rays observed near the earth. In the middle of 1964 ASm~mGE et al. (1.967) made an analysis of cosmic-ray intensity observed on the