Will Solar Orbiter allow to separate convected structures from propagating fluctuations within the solar wind turbulence?

Recent results obtained from the analysis of interplanetary observations recorded by Helios 2 at 0.3 AU showed, for the first time, that the Probability Distribution Function of magnetic field vector differences within the MHD frequency range of turbulence can be remarkably well fitted by a double log-normal. These two components of the total PDF have been ascribed to Alfvénic fluctuations and convected structures. This analysis, which needs high time resolution data to be performed, was carried on using only magnetic field data since plasma measurements were at much lower time resolution. Consequently, we lack of a sure proof of the Alfvénic nature of those fluctuations that we believe contribute to one of the two lognormals. The second lognormal should be due to convected structures but, whether these structures are locally generated by the turbulent evolution of the fluctuations or they rather come from the source regions of the wind, where they reflect the complicate topology of the magnetic field, is still unknown. High time resolution in-situ observations performed by Solar Orbiter at the perihelion, during the corotation phase, would certainly amplify the results already reached by Helios would finally give an answer to these problems. In particular, while in-situ measurements would allow to test the Alfvénic nature of the fluctuations, high spatial resolution remote sensing would help to disentangle spatial from temporal effects allowing to recognize whether convected structures come directly from the sun or they rather are a by-product of the turbulent evolution of interplanetary fluctuations.