Magnetic Structure of Halo CMEs and Corresponding ICMEs

Details Magnetic Structure of Halo CMEs and Corresponding ICMEs Magnetic Structure of Halo CMEs and Corresponding ICMEs

Dec 2005

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2005agufmsh13a0300k&link_type=abstract

American Geophysical Union, Fall Meeting 2005, abstract #SH13A-0300

Physics

2111 Ejecta, Driver Gases, And Magnetic Clouds, 7513 Coronal Mass Ejections (2101), 7959 Models

Scientific paper

The detailed connection between a halo coronal mass ejection (CME) and its corresponding ``interplanetary CME'' (ICME) is an area of active study. Using the erupting flux rope model [1-2], we present model/data comparisons for multiple CME/ICME events near the sun (using coronagraph image data) and in the heliosphere (using in situ measurements). We find that the near-Sun magnetic configuration, as obtained from a match of the model to the observed halo-CME morphology, is closely related to the ICME magnetic configuration, as determined by matching the model ICME to the in situ magnetic field and plasma measurements. The differences between the near-Sun flux-rope orientation parameters and the near-Earth orientation parameters are noted in each case. These indicate that, typically, the apex of the flux rope is deflected by 5-10 degrees as the flux rope expands outwards to 1 AU. [1] Chen, J. 1996, JGR, 101, 27499 [2] Krall, J. et al., 2000, ApJ, 539, 964

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