Speaker
Description
First Name: Raffaella
Last Name: D'Amicis
Email Address: raffaella.damicis@inaf.it
Affiliation: INAF - IAPS
All Authors: R. D’Amicis, D. Trotta, O. Dhamane, A. Larosa, S. Benella, S. Yardley, R. De Marco, M. Laurenza, L. Sorriso-Valvo, D. Turner, D. Perrone, M. Velli, O. Panasenco, R. Bruno, D. Telloni, C. Owen, P. Louarn, S. Livi, J. Rodriguez-Pacheco, R. Wimmer-Schweingruber, T. Horbury
Abstract: Alfvénic fluctuations are ubiquitous in the solar wind and are thought to play a key role in several heliospheric processes, such as solar wind heating and acceleration, energetic particle acceleration, cosmic ray propagation, and geomagnetic activity. The ESA/NASA Solar Orbiter mission offers a unique opportunity to investigate the properties and origin of Alfvénic streams and their radial evolution. Owing to its orbital configuration, Solar Orbiter crosses the Sun–Earth line approximately once per year, enabling direct comparison with in-situ measurements detected at L1. We present a coordinated analysis of an Alfvénic slow wind stream observed by Solar Orbiter and Wind, subsequently overtaken by an ICME with a supercritical fast forward shock at its leading edge, propagating at ~ 1000 km/s at both spacecraft. Ballistic backmapping combined with high-resolution remote sensing observations allows us to identify its solar source region. Measurements from Solar Orbiter and Wind provide a robust framework to investigate the radial evolution of the stream’s turbulent properties, to assess the mechanisms responsible for the evolution of Alfvénicity and to address how the shock system evolves, focusing on the transmission of such Alfvénic fluctuations from up- to downstream at both heliocentric distances. We finally address the role of such a complex magnetic environment in the acceleration and variability of high energy (>1 MeV) protons, observed at both Solar Orbiter and Wind. These results offer new insights into the coupled evolution of turbulence, shocks, and energetic particles in the inner heliosphere.