In this period researchers conceptualized the magnetosphere as a single, globally interconnected system in which convection is driven by solar wind forcing and the structure of the interplanetary magnetic field. There was a strong emphasis on linking auroral activity, geomagnetic disturbances, and ionospheric electron distributions to large-scale, organized plasma flows, with an initial shift toward global-scale modeling and energy transfer pathways. Methodologically, early satellite observations and theoretical frameworks supported a picture of solar wind energy entering near-Earth space through convection-driven circulation and field-aligned currents.