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We analyze the complete chain of effects caused by a solar eruptive event inorder to better understand the dynamic evolution of magnetic-field relatedquantities in interplanetary space, in particular that of magnetic flux andhelicity. We study a series of connected events (a confined C4.5 flare, aflare-less filament eruption and a double-peak M-class flare) that originatedin NOAA active region (AR) 12891 on 2021 November 1 and November 2. We deducethe magnetic structure of AR 12891 using stereoscopy and nonlinear force-free(NLFF) magnetic field modeling, allowing us to identify a coronal flux rope andto estimate its axial flux and helicity. Additionally, we compute reconnectionfluxes based on flare ribbon and coronal dimming signatures from remote sensingimagery. Comparison to corresponding quantities of the associated magneticcloud (MC), deduced from in-situ measurements from Solar Orbiter and near-Earthspacecraft, allows us to draw conclusions on the evolution of the associatedinterplanetary coronal mass ejection (ICME). The latter are aided through theapplication of geometric fitting techniques (graduated cylindrical shellmodeling; GCS) and interplanetary propagation models (drag based ensemblemodeling; DBEM) to the ICME. NLFF modeling suggests the host AR's magneticstructure in the form of a left-handed (negative-helicity) sheared arcade/fluxrope reaching to altitudes of 8-10 Mm above photospheric levels, in closeagreement with the corresponding stereoscopic estimate. Revealed from GCS andDBEM modeling, the ejected flux rope propagated in a self-similar expandingmanner through interplanetary space. Comparison of magnetic fluxes andhelicities processed by magnetic reconnection in the solar source region andthe respective budgets of the MC indicate a considerable contribution from theeruptive process, though the pre-eruptive budgets appear of relevance too.

Tracking magnetic flux and helicity from Sun to Earth -- Multi-spacecraft analysis of a magnetic cloud and its solar source