lundi 17 juin 2019, par Xin Cheng (School of Astronomy and Space Science, Nanjing University& Max Planck Institute for Solar System Research)
Vendredi 21 juin 2019 à 14h00 , Lieu : Salle de confĂ©rence du bâtiment 17
Coronal mass ejections (CMEs) and solar flares are the large-scale and most energetic eruptive phenomena in the solar system and able to release a large quantity of high-speed plasma and magnetic flux into the solar wind, probably seriously affect the safety of human high-tech activities in outer space. Nevertheless, the key questions of how and when CMEs/flares are initiated are still puzzled. Very importantly, the AIA data show that the pre-eruptive configuration of CMEs/flares may appear as a coherent plasma channel structure with a temperature up to 10 million degree, even pre-existing prior to the eruption. This thus allows us to decipher the physics during the initiation and early phase of solar eruptions. In this talk, I will first present observational features of magnetic reconnection during the slow rise phase that plays an important role in creating and heating the pre-existing flux rope. For the second part, I will talk some common behaviours of the early evolution of solar eruptions, which probably can be used to distinguish different CME/flare models.
