engleski

Coronal Mass Ejection of 26 February 2000: Complete Analysis of the Three-part CME Structure

We analyze the kinematics and morphology of the limb coronal mass ejection (CME) of 26 February 2000, utilizing observations from Mauna Loa Solar Observatory (MLSO), the Solar and Heliospheric Observatory (SOHO) and the Geostationary Operational Environmental Satellite (GOES). Also, we analyze the relation between dynamics of the CME and the energy release in the associated flare. An intricate structure (prominence, prominence-like absorbing feature, cavity and bright overlying arcade) is clearly recognizable in the low corona during the pre-eruption phase of slow rise. This provided measurements of kinematics of verious features from the very beginning of the eruption up to the post-acceleration phase which was followed up to 32 solar radii. Such events are observed only occasionaly, and are of great importance for the comprehension of the nature of forces driving CMEs. The acceleration maximum was attained at the radial distance of 2.4 solar radii from the solar center and ceased beyond 12 solar radii. The time profiles of the acceleration of various features of CME are showing "self-similar" expansion and implying a common driver. The acceleration phase was synchronized to a certain degree with the impulsive phase of the associated two-ribbon flare. Observations provide clear evidence that CME eruption caused a global restructuring of the magnetic field in the outer and inner corona. Furthermore, kinematics and morphological properties of this CME show possibility that in some events the prominence can evolve into a structure which looks like three-part structure CME, i.e. where the frontal rim is just a part of helically twisted prominence.

Sun: coronal mass ejection; MHD

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