Dynamics of Flux-Rope CMEs: SECCHI Observation and Theory

Statistics – Applications

Scientific paper

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7513 Coronal Mass Ejections (2101), 7514 Energetic Particles (2114), 7519 Flares

Scientific paper

The physical mechanism responsible for the acceleration and propagation of CMEs through the corona and interplanetary medium has been an important open question of solar-heliospheric physics. Often associated with CMEs are SEPs and flares. The physical connections between CMEs and these phenomena are also major questions. The new SECCHI observations represent unprecedented opportunities to test and establish new understanding of CME physics both closer to and farther away from the Sun than was previously possible. The LASCO observations have established that most, if not all, CMEs can be understood as expanding magnetic flux ropes. Much work has been done to understand flux-rope dynamics based on this hypothesis. In particular, the erupting flux-rope model has been extensively tested against LASCO data with good agreement. In this talk, I will discuss new results from recent applications of this theoretical model to SECCHI EUVI, COR-1, COR-2, and HI-1 observation. Several CMEs and their dynamics observed to about 100 R&sun; (projected) have been studied. Forces acting on these CMEs are discussed for both the inner-corona and heliospheric regions. It is shown that the erupting flux-rope model is able to fit the observed CME trajectories throughout the EUVI-COR1-COR2-HI1 field of view, indicating that the model correctly captures the basic physics, i.e., forces and magnetic geometry, of acceleration and propagation of CMEs. It is found that significantly larger values of the drag coefficient in the model than previously used are required to fit both the COR-1/COR-2 data and HI-1 data. Thus, the new expanded field of view of SECCHI imposes stronger constraints on model parameters than does the previous LASCO data set. It is also shown that the duration of the poloidal flux injection functions chosen to fit the CME trajectory closely match the duration of the observed GOES X-ray light curves for both short-duration and long-duration flares. The velocity components of the 3D flux rope parallel and perpendicular to the Archimedean spiral magnetic field are calculated along the CME trajectory. Possible physical connections of CMEs to flare energy release and shock acceleration of SEPs are discussed, suggesting a unified way to understand these related phenomena. Work supported by ONR and NASA

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