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This study focuses on the role that magnetically dominated\udfluctuations have within the solar wind MHD turbulence. It is\udwell known that, as the wind expands, magnetic energy starts to\uddominate over kinetic energy but we lack of a statistical study\udapt to estimate the relevance of these fluctuations depending on\udwind speed, radial distance from the sun and heliographic\udlatitude. Our results suggest that this kind of fluctuations can\udbe interpreted as non-propagating structures, advected by the\udwind during its expansion. In particular, observations performed\udin the ecliptic revealed a clear radial dependence of these\udmagnetic structures within fast wind, but not within slow wind.\udAt short heliocentric distances (~0.3 AU) the turbulent\udpopulation is largely dominated by Alfvénic fluctuations\udcharacterized by high values of normalized cross-helicity and a\udremarkable level of energy equipartition. However, as the wind\udexpands, a new-born population, characterized by lower values of\udAlfvénicity and a clear imbalance in favor of magnetic energy\udbecomes visible and clearly distinguishable from the Alfvénic\udpopulation largely characterized by an outward sense of\udpropagation. We estimate that more than 20% of all the\udanalyzed intervals of hourly scale within fast wind are\udcharacterized by normalized cross-helicity close to zero and\udmagnetic energy largely dominating over kinetic energy. Most of\udthese advected magnetic structures result to be non-compressive\udand might represent the crossing of the border between adjacent\udflux tubes forming, as suggested in literature, the advected\udbackground structure of the interplanetary magnetic field. On the\udother hand, their features are also well fitted by the Magnetic\udField Directional Turnings paradigm as proposed in literature

Magnetically dominated structures as an important component of the solar wind turbulence