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Abstract:
The Solar wind transports plasma and magnetic field from the low solar atmosphere to the outer Heliosphere in a highly fluctuating way that goes from small structured streams (the so called spaguettis) to large structures as high speed streamers and interplanetary coronal mass ejections. The identification of such structures in the in situ data has been a difficult task at one astronomical unit (by Wind, ACE and DSCOVR spacecraft) and it is worse at lower heliospheric distances available now with missions such as Parker Solar Probe and Solar Orbiter. Usually, this identification method is time-consuming and ambiguous as it relies on the observer's judgement which also neglects structure characteristics caused by evolution and propagation through more complex ambient solar wind. In this work, we present a statistical study of typical fluctuation of the solar wind parameters that can be used as a tracer to automatically identify the arrival of large scale structures in the solar wind at any distances from several solar radii to 1 AU and beyond. We propose a methodology to discern between solely structures traveling into the interplanetary medium or complex ones formed after the interaction between two or more large scale structures.
