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Flux rope axis geometry of magnetic clouds deduced from in situ data

Published online by Cambridge University Press:  06 January 2014

Miho Janvier
Affiliation:
Observatoire de Paris, LESIA, UMR 8109 (CNRS), F-92195 Meudon Principal Cedex, France email: miho.janvier@obspm.fr, pascal.demoulin@obspm.fr
Pascal Démoulin
Affiliation:
Observatoire de Paris, LESIA, UMR 8109 (CNRS), F-92195 Meudon Principal Cedex, France email: miho.janvier@obspm.fr, pascal.demoulin@obspm.fr
Sergio Dasso
Affiliation:
Departamento de Física e Instituto de Astronomía y Física del Espacio (UBA-CONICET), Facultad de Ciencias Exactas y Naturales, Universidad de Buenos Aires, 1428 Buenos Aires, Argentina email: dasso@df.uba.ar
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Abstract

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Magnetic clouds (MCs) consist of flux ropes that are ejected from the low solar corona during eruptive flares. Following their ejection, they propagate in the interplanetary medium where they can be detected by in situ instruments and heliospheric imagers onboard spacecraft. Although in situ measurements give a wide range of data, these only depict the nature of the MC along the unidirectional trajectory crossing of a spacecraft. As such, direct 3D measurements of MC characteristics are impossible. From a statistical analysis of a wide range of MCs detected at 1 AU by the Wind spacecraft, we propose different methods to deduce the most probable magnetic cloud axis shape. These methods include the comparison of synthetic distributions with observed distributions of the axis orientation, as well as the direct integration of observed probability distribution to deduce the global MC axis shape. The overall shape given by those two methods is then compared with 2D heliospheric images of a propagating MC and we find similar geometrical features.

Type
Contributed Papers
Copyright
Copyright © International Astronomical Union 2013 

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