Physics
Scientific paper
Dec 2003
adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2003agufmsh42b0519c&link_type=abstract
American Geophysical Union, Fall Meeting 2003, abstract #SH42B-0519
Physics
7509 Corona, 7524 Magnetic Fields, 7594 Instruments And Techniques
Scientific paper
Theoretical modeling of the dynamics of coronal mass ejections (CMEs) has progressed to the point where calculated CME acceleration and speed can be quantitatively compared with observed data (e.g., TRACE, MK3, and C1--C2 data). However, the coronal magnetic fields underlying CMEs and their evolution have not been accurately observed. Nevertheless, the magnetic fields of CMEs are indirectly known by in situ measurements of their presumed interplanetary counterparts. Anticipating improved future measurements and the increasing importance of the CME phenomenon in terms of Sun-Earth connection, we investigate the magnetic fields of CMEs and their evolution to 1 AU. For this purpose, we use a flux-rope model of CMEs that has been extensively tested against observed CMEs with good agreement: (1) we will construct an ensemble of equilibrium flux ropes imbedded in a range of overlying coronal magnetic field; (2) we then allow the flux ropes to erupt and propagate to 1 AU through the corona and the interplanetary medium. We calculate the initial magnetic field of a CME based on its geometrical size (e.g., using the length of a magnetic neutral line obtained from magnetogram data as a proxy for the footpoint separation distance). For various scenarios with or without injection of poloidal magnetic flux into the initial flux rope, we quantitatively determine the range of coronal magnetic field that yields realistic CME dynamics within 30 Rsun and that results in magnetic fields at 1 AU that are consistent with those of observed magnetic clouds. We discuss predicted magnetic field signatures in the photosphere, the corona, and at 1 AU for a number of distinct scenarios. Work supported by ONR and NASA
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