Magnetic Topology of in and out of Ecliptic ICME Events: ULYSSES/HI-SCALE and ACE/EPAM observations

Physics

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7513 Coronal Mass Ejections, 7514 Energetic Particles (2114), 2100 Interplanetary Physics, 2114 Energetic Particles, Heliospheric (7514), 2134 Interplanetary Magnetic Fields

Scientific paper

In January 2000, ULYSSES observed an Interplanetary Coronal Mass Ejection (ICME) event at 43° S heliolatitude and ~4.1 AU helioradius. We use electron (Ee>38 keV)observations by the ULYSSES/HI-SCALE experiment to trace the large-scale structure and topology of the Interplanetary Magnetic Field (IMF) embedded within the ICME. The still controversial issue of whether ICMEs have been detached from the solar corona or are still magnetically anchored to it when they arrive at the spacecraft is addressed. Based upon the time evolution of the angular distributions of the particle intensities we infer that the ICME involved complex intertwined structures including regions both connected to and disconnected from the Sun. The detection of counterstreaming solar electrons in a portion of the ICME is consistent with the trapping of the injected electrons within closed magnetic structures. The observation by the ACE/EPAM experiment of two impulsive solar flare electron events inside an in ecliptic ICME in May 1998 suggests that field lines threading through the ICME are rooted at the Sun. The observed anisotropy characteristics are consistent with the magnetic topology of a magnetic bottle between a magnetic mirror located at the Sun and a magnetic constriction upstream from ACE formed by the convergence of open field lines that reflects the outgoing electrons. The magnetic mirror strength is calculated in one case based upon the local IMF observations and the electron pitch-angle distributions. A magnetic field enhancement observed by ACE in the downstream region of the CME-driven shock is identified as the agent responsible for the mirroring of the energetic electrons.

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