A robust estimation of the twist distribution in magnetic clouds

¹ Universidad de Buenos Aires, Facultad de Ciencias Exactas y Naturales, Departamento de Ciencias de la Atmósfera y los Océanos (DCAO), Laboratorio de Meteorología del esPacio (LAMP), 1428 Buenos Aires, Argentina
e-mail: vlanabere@at.fcen.uba.ar
² LESIA, Observatoire de Paris, Université PSL, CNRS, Sorbonne Université, Université Paris-Cité, 5 place Jules Janssen, 92195 Meudon, France
³ Laboratoire Cogitamus, 1 3/4 rue Descartes, 75005 Paris, France
e-mail: pascal.Demoulin@obspm.fr
⁴ CONICET, Universidad de Buenos Aires, Instituto de Astronomía y Física del Espacio (IAFE), Laboratorio de Meteorología del esPacio (LAMP), CC. 67, Suc. 28, 1428 Buenos Aires, Argentina
e-mail: sdasso@iafe.uba.ar

Received: 26 September 2022
Accepted: 24 October 2022

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%.