A robust estimation of the twist distribution in magnetic clouds

TL;DR

This study uses a refined superposed epoch analysis to robustly determine the magnetic twist distribution in magnetic clouds, revealing a nearly uniform core twist with a steep border increase, and confirms previous findings with improved accuracy.

Contribution

The paper introduces a new approach using flux rope model fitting to select the closest approach time, reducing biases and improving the accuracy of twist distribution measurements in magnetic clouds.

Findings

The twist profile is nearly uniform in the core.

A steep increase in twist occurs at the flux rope border.

Results confirm previous findings with a 20% larger twist estimate.

Abstract

Magnetic clouds (MCs) are observed insitu 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. 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. 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. 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 $\sim 20\%$.