Other
Scientific paper
Dec 2008
adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2008agufmsh22a..08z&link_type=abstract
American Geophysical Union, Fall Meeting 2008, abstract #SH22A-08
Other
7509 Corona, 7513 Coronal Mass Ejections (2101), 7514 Energetic Particles (2114), 7519 Flares, 7524 Magnetic Fields
Scientific paper
Observations at 1 AU indicate that only 1/3 of coronal mass ejections (CMEs) have a flux-rope structure, while other 2/3 of CMEs have a complex disordered magnetic field. The initiation of the flux-rope CMEs has been extensively simulated with various magnetohydrodynamic (MHD) models. However, the initiation of the non-flux-rope CMEs is rarely done in numerical modeling. Recently, we have numerically simulated the physical origin and characteristics of the non-flux-rope CMEs by using a three-dimensional axisymmetric time- dependent self-consistent MHD model. The results show that the emergence of counter-clockwise flux rope from the photosphere at the open field region, near the closed magnetic field lines, can initiate a magnetic configuration which produces the magnetic reconnection at the coronal base. Physically, the magnetic field of the emerged counter-clockwise flux rope has anti-polarity with the background open field and the location of the magnetic flux emergence is at the edge of a coronal hole. This magnetic reconnection between closed and open field lines at the coronal base generates an Alfvenic jet-like plasma outflow, which can be developed into a non-flux-rope CME, if enough magnetic energy deposits, with strong disturbances of the magnetic fields in the solar corona and interplanetary space. Solar energetic particle (SEP) events in association with the non-flux-rope CMEs are usually impulsive. In this presentation, we will present our MHD simulation results of non-flux-rope CMEs associated with the impulsive SEP events.
Tan Aihong
Wu Seongho
Zhang Tianmeng
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