Lessons Learned from Flux-ropes Observed by Wind spacecraft 1995-2015
Abstract
It is well known that the geoeffectiveness of interplanetary coronal mass ejections (ICMEs) depends on their magnetic field topology and global geometry. The observed in-situ magnetic signatures are more complex than a simple flux-rope magnetic topology. Sometimes these events are called Ejectas or Magnetic flux-rope like. On the other hand, imaging observations of CMEs close to the Sun suggest that the entrained flux-rope undergo significant evolutionary changes, such as deformation or distortion, during their heliospheric propagation.
The goal of this paper is to explore the magnetic field and plasma parameter observations in order to get information about the magnetic field configuration, structure and geometry of the magnetic obstacles embedded in the ICMEs. This goal can be also spread on questions as: Can we quantify the Flux-Rope distortion at any heliospheric distance? Can we predict axial curvature or deformations? How is the expansion affecting to the compression in the magnetic obstacle front? Can we find any relationship between the magnetic field strength compression and the expansion velocity?. The answers to these questions will aid to address the final question: can we quantify the forces that govern the ICME evolution? To accomplish this study, we have selected Earth-directed CMEs observed by in-situ instruments onboard on Wind spacecraft (wind.nasa.gov) in the period 1995-2015.- Publication:
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Solar Heliospheric and INterplanetary Environment (SHINE 2016)
- Pub Date:
- July 2016
- Bibcode:
- 2016shin.confE..59N