Nuovo Cimento Suppi. 22, 321,1961; Leighton, R., Noyes, R., and Simon, G. Astrophys. J. 135, 474, 1962), large-scale, principally horizontal, motions have been observed in the solar photospliere. These motions have a cellular appearance, ai~d the flow proceeds from the center of each "cell" toward the outer boundary, with velocities of 0.3-0.5 km/sec. These cells are arranged in a more-or-less regular pattern over the solar surface, with an average cell diameter of 3.0-3.5 X 10~ km. Cross-correlation measurements obtained by superposition of velocity plates and Ca+(X3933) plates show that the K2,3 emission network occurs directly above the boundaries of the velocity cells. Downward velocities of 1.0-2.0 km/sec are observed in the wings of Ha (Ax=0.7 A) and HP (AX=0.4A). These localized motions exist in a network pattern which coincides with the position of the K2,3 emission and the velocity cell boundaries. The lifetime of the K2,3 network has been measured by cross-correlating plates taken at various time intervals and has a mean life of 17-21 h in excellent agreement with the finding of C. Macris (Mcm. Soc. Astron. Ital. 33, 85,1962). Using magnetograph measurements obtained by R. Howard (Astrophys. J. 130, 193, 1959), we find a very high degree of correlation between the positions of weak magnetic fields (1.5-5.0 G) and the K2,3 network. The probability that the observed correlation is a random statistical ~uctuation is 10-~. For stronger fields (>~ 5 G) the corresponding probability is less than 10-11. These observations suggest that the average solar magnetic field (0.5-1.0 G) is swept to the cell boundaries by the horizontal currents, and concentrates there in strengths perhaps two to ten times greater than the average field. These narrow regions of enhanced field strength could then account for the presence of the K2,3 emission at the cell boundaries, and perhaps also for the downflow of chromospheric material in this region, as well as small "dots" of rising material seen at the edges of the downward flowing network, which may be spicules seen on the disk. This work was assisted by the Office of Naval Research.