Previous observations of magnetic pulsations in space have not been able to distinguish temporal from spatial structure unambigously. Using the ISEE 1 and 2 spacecraft, satellites closely spaced in identical orbits, we are able to determine whether the observed amplitude variations are due to the motion of the spacecraft through a time stationary structure or are due to temporal changes in the wave. We have examined four dayside Pc 4, 5 period pulsations, three of which are observed between L = 4 and 7 within 10¿ of the magnetospheric equator. The resonant region widths of these three events range from ~0.2--1.6 L shells. These are the first direct measurements of resonant region widths in space. For two of the three near-equatorial events, plasma density data was available and indicated that the events are associated with gradients in the electron number density at the plasmapause. In one event, although waves are observed continuously by ISEE 2 during a portion of its inbound trajectory, at ISEE 1 there is a gap in the waves at the same time as a depleted density region is encountered. The gap in the waves can be explained as either a temporal or spatial effect, although the latter seems more likely. In addition to these observations we are able to use two independent techniques to determine the harmonic of two pulsation events. The first method compares the observed wave period with the period predicted by standing wave theory. The second method, which previously has been applied only indirectly, is to compare the phase of the observed wave electric and magnetic field. Alone neither of these methods can unambiguously determine the resonance harmonic. Here, using both methods together for the first time, we find that both events are second harmonic oscillations. This suggests that second harmonic oscillations are perhaps more common than previously thought.