Abstract
The Explorer 34 satellite was used as a platform for studying ultralow- frequency (ULF) magnetic waves from 0.01 to 0.2 Hz in the plasma sheet. The power spectral density was found to be proportional to the inverse square of the frequency in the plasma sheet and exhibited few, if any, significant spectral peaks. Further, the plasma sheet was characterized by power spectral density values that were higher than those of the high-latitude tail. The X/sub sm/, component where the subscript sm indicates solar magnetospheric coordinates, exhibited greater power spectral density values than the other two components. The most significant result, however, was that the power spectral density calculated for the frequency range 0.012-O.1 Hz in the plasma sheet increased from minimal values during quiet times to maximum levels during thc later stages of a substorin. It is shown that this result, in the frequency range studied, is probably inconsistent with the expectations of the substorm model of Hill and Dessler (1971), in which the plasma sheet was contained, during quiet times, by magnetic fluctuations.
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