Abstract
Previous analysis of magnetohydrodynamic-scale currents in high-speed solar wind near 1 AU suggests that the most intense current-carrying structures occur at electron scales and are characterized by average current densities on the order of $1~\mbox{pA}/\mbox{cm}^{2}$ . Here, this prediction is verified by examining the effects of the measurement bandwidth and/or measurement resolution on the analysis of synthetic solar wind signals. Assuming Taylor’s hypothesis holds for the energetically dominant fluctuations at kinetic scales, the results show that when $\nu_{c}\gg \nu_{b}$ , where $\nu_{c}$ is the measurement bandwidth and $\nu_{b} \approx 1/3~\mbox{Hz}$ is the break frequency, the average scale of the most intense fluctuations in the current density proxy is approximately $1/\nu_{c}$ , and the average peak current density is a weakly increasing function that scales approximately like $\nu_{c}^{0.1}$ .
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