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Magnetic field lines distribution inside magnetic clouds
Sergio Dasso - IAFE-DCAO-LAMP (UBA-CONICET); Vanina Lanabere - DCAO-LAMP (FCEN-UBA), Argentina; - 4LESIA, Observatoire de Paris, Université PSL, CNRS, France; Miho Janvier - 1Institut d'Astrophysique Spatiale, CNRS, Université Paris-Sud, Université Paris-Saclay, Orsay, France; Luciano Rodriguez - Solar–Terrestrial Center of Excellence – SIDC, ROB, Belgium; - IAFE (UBA-CONICET), Argentina
The internal distribution of the magnetic twist forming the flux rope of MCs (i.e., the number of turns per unit length), is a key property to link MCs with their solar origin and ejection processes, to unveil the MCs equilibrium state (e.g., the magnetic tension), and also to better understand the internal energetic particle propagation. Estimating the magnetic twist from 'in situ' observations and using a single event, has a major difficulty produced by the significant field fluctuations: the significant increase of the noise in the observed B time series. Thus, the strong bias of the deduced twist.
In this work, we apply a superposed epoch analysis to a significant sample of MCs observed at 1 au, to extract their common features, and to remove the peculiarity of individual cases. From this analysis, we quantify the typical twist distribution inside the flux ropes forming MCs. As main results, we find that the twist is nearly uniform in the core (central half part), and it increases moderately, up to a factor two, towards the MC boundaries.
16 July 2020
Abstract submission opens:
16 July 2020
European Space Weather Medals:
6 September 2020
25 September 2020
Registration deadline: [extended]
10 October 2020
Abstract submission deadline:
4 September 2020