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Structures of Interplanetary Magnetic Flux Ropes and Comparison with Their Solar Sources View all abstracts by submitter

qiang hu   Submitted: 2014-07-21 20:34

During the process of magnetic flux rope ejection, magnetic reconnection is essential to release the flux rope. The question remains: how does the magnetic reconnection change the flux rope structure? In this work, we continue with the original study by Qiu et al. (2007) by using a larger sample of flare-CME-ICME events to compare properties of ICME/MC flux ropes measured at 1 AU and properties of associated solar progenitors including flares, filaments, and CMEs. In particular, the magnetic field-line twist distribution within interplanetary magnetic flux ropes is systematically derived and examined. Our analysis shows that, similar to what was found before, for most of these events, the amount of twisted flux per AU in MCs is comparable with the total reconnection flux on the Sun, and the sign of the MC helicity is consistent with the sign of helicity of the solar source region judged from the geometry of postflare loops. Remarkably, we find that about one half of the 18 magnetic flux ropes, most of them being associated with erupting filaments, have a nearly uniform and relatively low twist distribution from the axis to the edge, and the majority of the other flux ropes exhibit very high twist near the axis, of up to >=5 turns per AU, which decreases toward the edge. The flux ropes are therefore not linear force free. We also conduct detailed case studies showing the contrast of two events with distinct twist distribution in MCs as well as different flare and dimming characteristics in solar source regions, and discuss how reconnection geometry reflected in flare morphology may be related to the structure of the flux rope formed on the Sun.

Authors: Qiang Hu, Jiong Qiu, B. Dasgupta, A. Khare, and G. M. Webb
Projects: ACE,GOES X-rays ,SDO-AIA,SDO-HMI,SoHO-EIT,SoHO-LASCO,STEREO,Wind

Publication Status: accepted by ApJ
Last Modified: 2014-08-08 09:08
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