Speaker
Description
We aim to develop a more coherent understanding of the evolution of the physical properties of solar eruptions as they propagate through interplanetary space. Recent multi-spacecraft observations of single ICME events allow us to systematically trace magnetic field related properties across vast spatial domains. Among these properties, magnetic helicity appears to be especially interesting. As a quasi-conserved quantity, magnetic helicity effectively captures the complexity of the magnetic field—specifically its shear and twist—allowing for consistent tracking from the solar atmosphere to interplanetary space.
We present an analysis of the flare/CME event SOL2024-03-23T X1.1 as well as of the global flux rope structure of the associated ICME event that impacted Solar Orbiter at a heliocentric distance of 0.39 AU, BepiColombo at 0.58 AU, STEREO-A at 0.96 AU, as well as Wind at 0.99 AU.
To model the 3D coronal magnetic field of the solar source active region (NOAA 13614), we employ non-linear force-free field (NLFF) modelling using a newly developed machine learning-based approach (NF2). To reconstruct the flux rope parameters of the associated ICME, we apply the semi-empirical 3DCORE model, which enables the reconstruction of ICME magnetic properties as functions of interplanetary distance and time, based on in-situ measurements from BepiColombo, Solar Orbiter, Wind and STEREO-A. From the reconstructed magnetic field data, we calculate the corresponding magnetic helicity values and compare them to those derived from the solar source region. This analysis provides a spatially resolved assessment of magnetic helicity, allowing us to track its evolution from the Sun to near-Earth space. Our goal is to establish consistent and physically meaningful helicity estimates across multiple observational domains.
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