A robust estimation of the twist distribution in magnetic clouds

Abstract

Context. Magnetic clouds (MCs) are observed in situ by spacecraft. The rotation of their magnetic field is typically interpreted as the crossing of a twisted magnetic flux tube, or flux rope, which was launched from the solar corona. Aims. The detailed magnetic measurements across MCs permit us to infer the flux rope characteristics. Still, the precise spatial distribution of the magnetic twist is challenging, and thus is debated. Methods. In order to improve the robustness of the results, we performed a superposed epoch analysis (SEA) of a set of well observed MCs at 1 au. While previous work was done using the MC central time, we here used the result of a fitted flux rope model to select the time of the closest approach to the flux rope axis. This implies a precise separation of the in-and outbound regions to coherently phase the observed signals. We also searched for and minimised the possible biases such as magnetic asymmetry and a finite impact parameter.Results. We applied the SEA to derive the median profiles both for the flux rope remaining when crossed by the spacecraft and to recover the one present before erosion. In particular, the median azimuthal B component is nearly a linear function of the radius. More generally, the results confirm our previous results realised without such a deep analysis. The twist profile is nearly uniform in the flux rope core, with a steep increase at the border of the flux rope and with similar profiles in the in-and outbound regions. The main difference with our previous study is a larger twist by ∼ 20%.

On the Role of Alfvénic Fluctuations as Mediators of Coherence within Interplanetary Coronal Mass Ejections: Investigation of Multi-spacecraft Measurements at 1 au

“…No statistically significant correlation/anticorrelation is found for B int (0.17 and 0.06 with p-value larger than 5% for Wind/SWE and ACE, respectively), corresponding to the direction of the flux-rope axis. Because the magnetic field component aligned with the direction of propagation of AFs is expected to be the least affected by fluctuations, such a picture may suggest that AFs are globally propagating primarily along the flux-rope axis (along B int , which typically constitutes the dominant magnetic field component within ICME flux ropes; see, e.g., Hu et al 2015;Lanabere et al 2020Lanabere et al , 2022 and manifest the larger anticorrelation in the other two magnetic field components (B min and B max ).…”