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Session 8 - Corona III.
Oral session, Saturday, June 28
Ballroom A, Chair: Barry LaBonte
While the WIND spacecraft at 1 AU was inside the magnetic cloud of October 18-20, 1995, five solar impulsive \sim1-10^2 keV electron events were observed by the 3-D Plasma and Energetic particles experiment. The solar type III radio bursts produced by these electrons can be directly traced from \sim1 AU back to x-ray flares at the Sun, providing the first direct identification of the footpoints of the cloud magnetic fields. One leg of this cloud clearly connects to a solar active region, AR 7912. The total magnetic flux within the cloud is estimated to be 10^13 Webers, implying that about 25% of the active region magnetic flux ( 4 x 10^13 Webers) is ejected in the cloud. Analysis of the arrival times of the electrons show that the lengths of the magnetic field lines in that leg vary from \sim4 AU near the cloud exterior to \sim1.5 AU near the cloud center, consistent with a force-free helical flux rope with \sim8 turns total on the outside. The length of smooth Archimedean spiral (\sim1.15 AU) predicted for the observed solar wind speed of \sim420 km/s, suggesting that the cloud may have expanded sideways (non-radially). Both the \sim0.1 - 1 keV solar wind heat flux electrons and \sim 1-10^2 keV energetic electrons show numerous simultaneous abrupt changes in flux level and anisotropy, from bidirectional streaming to unidirectional streaming to complete dropouts within the cloud. We interpret these as evidence for patchy disconnection of one end or both ends of cloud magnetic field lines from the Sun, most likely due to magnetic reconnection occurring after the cloud was ejected.
Program listing for Saturday