3-D Magnetic Field Geometry of the October 28, 2003 ICME: Comparison with SMEI White-Light Observations

Details 3-D Magnetic Field Geometry of the October 28, 2003 ICME: Comparison with SMEI White-Light Observations 3-D Magnetic Field Geometry of the October 28, 2003 ICME: Comparison with SMEI White-Light Observations

Dec 2006

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2006agufmsh33a0397j&link_type=abstract

American Geophysical Union, Fall Meeting 2006, abstract #SH33A-0397

Astronomy and Astrophysics

Astronomy

6023 Comets: Dust Tails And Trails (6210), 7513 Coronal Mass Ejections (2101), 7539 Stellar Astronomy, 7924 Forecasting (2722), 7954 Magnetic Storms (2788)

Scientific paper

Multiple reconstructions of the October 28-29, 2003 CME/ICME using white-light observations, ground-based cosmic-ray and in situ magnetic field flux rope modeling show two possible flux-rope configurations that pass Earth on opposite sides of the central symmetry axis of the disturbance. An analysis of flux rope model geometries initiated over a wide range in parameter space to test the uniqueness of the single spacecraft inversion reveals the fit is degenerate over a range of impact parameters such that two solutions are obtained. In one case (fit A) the disturbance passes Earth to the west of the rope center with the rope axis at a low inclination of 20 deg to the ecliptic, similar to the ground-based flux rope analysis by Kuwabara et al.~(2004). In the second case (fit B) the disturbance passes Earth to the east of the flux rope axis, with the rope axis more highly inclined at 42 deg from the ecliptic, consistent with the SMEI white-light analysis of Jackson et al.~(2006). The current densities in both solutions indicate a nearly force-free structure. Multipoint studies of ICMEs show the radius of curvature in the plane of the rope is between that of a dipole field line connected to the Sun and that of a circular field line connected to the Sun. Assuming a dipole field geometry for the large- scale axial field curvature of the rope results in a 3-D reconstruction for case B that is consistent with the loop structure and observed speed in the white-light LASCO images and SMEI density reconstruction, but not for case A. Multipoint measurements of large-scale solar wind transients is one of the key objectives of the Stereo mission, allowing more accurate 3-D reconstructions of in situ data for comparison with white-light observations. Until they become available, the large-scale axial field orientation and loop geometry of these rope reconstructions provides another tool to constrain magnetic flux rope fits of ICMEs using single spacecraft measurements.

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