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Previous analyses have shown that polar wind fluctuations at MHD scales appear as a\udmixture of Alfvénic fluctuations and variations with an energy imbalance in\udfavour of the magnetic term. In the present study, by separately examining the\udbehaviour of kinetic and magnetic energies versus the Alfvénic correlation\udlevel, we unambiguously confirm that the second population is essentially\udrelated to a large increase of the magnetic energy with respect to that of\udthe Alfvénic population. The relevant new result is that this magnetic\udpopulation, though of secondary importance in terms of occurrence frequency,\udcorresponds to a primary peak in the distribution of total energy. The fact\udthat this holds in the case of polar wind, which is the least structured type\udof interplanetary plasma flow and with the slowest evolving Alfvénic turbulence,\udstrongly suggests the general conclusion that magnetic structures cannot be\udneglected when modeling fluctuations for all kinds of wind regime

On the distribution of energy versus Alfvénic correlation for polar wind fluctuations