Wuppertal 2015 – wissenschaftliches Programm
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EP: Fachverband Extraterrestrische Physik
EP 5: SDO/Sunrise/STEREO
EP 5.5: Vortrag
Dienstag, 10. März 2015, 18:30–18:45, G.10.02 (HS 9)
Radial Flow Pattern of a slow Coronal Mass Ejection — •Li Feng1,2, Bernd Inhester1, Weiqun Gan2, and Thomas Wiegelmann1 — 1Max Planck Institute for Solar System Research, Germany — 2Purple Mountain Observatory, China
Height-time plots of the leading edge of a coronal mass ejection (CME) have been often used to study its kinematics. A new method is proposed to analyze the CME kinematics in more details through its mass transport process. The method is able to estimate not only the CME speed at its front but also the radial flow speeds inside the CME. We have applied the method to a slow CME with an average leading edge speed about 487 km s−1. It is found that the radial flow speed increases with distance and decreases with time. CME mass increase is often attributed to two reasons: outflow from the dimming region and solar wind pile-up around the CME. The flow speed profiles of this slow CME reveals that the solar wind pile-up is improbable to make contributions to its mass. A further estimate of the CME kinetic energy indicates that the conventional kinetic energy derived from the total mass and leading edge speed can be two times larger than our value taking into account the internal mass and flow distributions. The Lagrangian trajectories derived from the obtained flow pattern for mass elements at different heights present much more information than the single leading-edge trajectory. We find that with time the leading edge trajectory gradually lag behind the trajectory of mass element with a fastest speed. It implies that the leading edge trajectory does not actually follow a material path as the name suggests.