The position of bright knots of 30 flares at their very beginning relative to the high-resolution isogauss maps of the longitudinal component (HII) and maps of the transverse component (H• of magnetic field are considered for seven days during the passage of the active and large spot group in Sept. 1963 (see Table I and maps on Figures 1-8).The flare bright knots occur simultaneously in regions of opposite magnetic polarity, and the majority of these knots are adjacent to neutral line Hif = 0, although not coinciding precisely with this line (Figure 9). Lenticular form of flare knots and the motions of bright material of flares is restrained by transversal field H• Also flares are closely associated (83 %) with so-called 'bifurcated regions', where specific crossing of transverse components takes place (Figures 4-5). There is wellexpressed (80 %) coincidence of flare knots with the strongest (positive or negative) electric currents as determined from the relation j = c/4zc rot H. The relation of results obtained to some existing theories of flares is briefly discussed.

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Abstract. s t a r has been compared with the interplanetary magnetic f i e l d observed with spacecraft near the earth, The mean photospheric magnetic field o f t h e sun seen as a Each change i n polarity of the mean solar f i e l d i s followed about 4* days later by a change i n polarity of the inter- has been compared w i t h observations of the interplanetary magnetic This methodThis m e a n solar f i e l d observed i n March through June f i e l d obtained w i t h the Ames Research Center magnetometers on t h e spacec r a f t Explorers 33 and 35, for which C. P. Sonett i s the Principal Investigator.Mihalov --e t al. (1968). The polarity of the interplanetary f i e l d was determined using the method described by Wilcox and Colburn (1969).plotted on the graph of solar observations taking account of the t r a n s i t time of solar wind plasma from sun t o earth, as described l a t e r i n t h i s paper. peaks; they W i l l be discussed l a t e r . ) expected behavior i s seen a t the peak a t a l a g of 4* + 27 days.peak i s considerably larger than would be expected; i n f a c t the absolute magnitude of t h i s peak i s l w g e r than the magnitude of the peak a t 4sdays. The explanation f o r the anamolous size of the peak a t 4+ -t 27 days m a y be found On the discussion of Schatten -- The result of such a delay Assume first t h a t the solar magnetic f i e l d i s stationary Then the resulting interplanetary magnetic sector pattern wouldLet us now change the polarity of a particular area i n theIn accordance with the above discussion we w i l l assume 7 .sector pattern, smewhat reduced, corresponding t o t h i s discrepancy i n the direction of t h e two fields.t i o n the corresponding change i n the interplanetary sector pattern w i l l have occurred, and similarly the correlation at 4-$ + 27 days will be back t o the full value.Then the correlation peak at a lag of 4* days w i l l be W e may further assume that i f we w a i t f o r one solar rota-W e may consider the meaning of the unshaded correlation peaks i n Figure 7 as a function of latitude corresponds t o the l a g of t h e cross-correlation peak i n Figure 8 as a function of latitude. Figure 8 shows the same property t h a t appeared i n the present investigation i n the discussion of Figure 4, namely t h a t the height of the crosscorrelation peak a t a l a g of 4+ -t 27 days i s larger than t h e height of the peak a t a lag of 4$ days. In Figure 8

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