Other
Scientific paper
May 2008
adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2008agusmsh21a..02l&link_type=abstract
American Geophysical Union, Spring Meeting 2008, abstract #SH21A-02
Other
2111 Ejecta, Driver Gases, And Magnetic Clouds, 2114 Energetic Particles (7514), 2134 Interplanetary Magnetic Fields, 2164 Solar Wind Plasma, 7513 Coronal Mass Ejections (2101)
Scientific paper
Coronal mass ejections (CMEs) are often assumed to be magnetic flux ropes, but direct proof has been lacking. A key feature, resulting from the translational symmetry of a flux rope, is that the total transverse pressure as well as the axial magnetic field has the same functional form over the vector potential along any crossing of the flux rope. We test this feature (and hence the flux-rope structure) by reconstructing the 22 May 2007 magnetic cloud (MC) observed at STEREO B, Wind/ACE and possibly STEREO A with the Grad-Shafranov (GS) method. The model output from reconstruction at STEREO B agrees fairly well with the magnetic field and thermal pressure observed at ACE/Wind; the separation between STEREO B and ACE/Wind is about 0.06 AU, almost half of the MC radial width. For the first time, we reproduce observations at one spacecraft with data from another well- separated spacecraft, which provides compelling evidence for the flux-rope geometry and is of importance for understanding CME initiation and propagation. The magnetic field line length, calculated from the velocity dispersion of energetic electrons within the MC, is substantially longer than the nominal Parker spiral field, which is consistent with a flux-rope structure. The reconstruction gives a global configuration of the MC at different spacecraft with a flattened cross section owing to the solar wind radial expansion. A similar approach is also performed with a force-free flux-rope fitting model in an effort to compare with the GS reconstruction results.
Bale Stuart
Galvin T.
Huttunen E.
Lin Runliang
Liu Ya-Ying
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