Multiple Flux Rope Events at the High-Latitude Magnetopause: CLSTER/RAPID Observation on January 26, 2001

Details Multiple Flux Rope Events at the High-Latitude Magnetopause: CLSTER/RAPID Observation on January 26, 2001 Multiple Flux Rope Events at the High-Latitude Magnetopause: CLSTER/RAPID Observation on January 26, 2001

Apr 2003

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2003eaeja.....2450p&link_type=abstract

EGS - AGU - EUG Joint Assembly, Abstracts from the meeting held in Nice, France, 6 - 11 April 2003, abstract #2450

Computer Science

Scientific paper

On January 26, 2001, the Cluster constellation traveled in northern duskside high-latitudes, crossing the cusp and magnetopause boundary regions, and entering the magnetosheath. Four Cluster spacecraft measurements during this outbound pass confirm that the cusp is a dynamic region full of energetic charged particles and turbulence and that energetic ion layer at high-latitudes outside of and adjacent to the duskside magnetopause exists when the IMF has a southward orientation. Multiple energetic ion flux bursts were observed in the energetic ion layer. The bursty enhancements of ion flux appear quasi-periodically with a repeated period being approximately 72 s. Two intense energetic ion bursts were also recorded later when the spacecraft encountered two FTEs in the magnetosheath. Each energetic ion flux burst was found to be closely related to a magnetic flux rope. The axes of the flux ropes lie in the direction pointing duskward/tailward and upward or nearly parallel to the ecliptic plane. An intense axis-aligned current flows inside the ropes with the current density reaching as high as ˜ 10-8A/m2. In each even, the main components of the energetic ions, which are protons, Helium and CNO ions originated from the magnetosphere, flow out into the magnetosheath along the axis of the flux rope. Meanwhile, the velocity of the magnetosheath thermal plasma relative to the HT frame is found to be basically along the axis of the flux rope also, but towards the magnetosphere. These flux ropes are likely to be produced via intermittent/quasi-periodic magnetic reconnection equatorward and dawnward of the Cluster location and move at similar HT velocities passing over the spacecraft.

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