JapaneseGEMSIS-Sun
Plasma Dynamics during a Solar Flare
A solar flare which strongly influences the local space weather is a long-standing problem in solar physics. The standard flare model predicts that magnetic reconnection occurs above the bright flare loops and hot fast flow should be located there. So far, various observations indicate the presence of hot fast flow above the flare loop. However, there is no imaging spectroscopic observation of the large solar flare at the solar limb. We studied the flare event occurred at the west solar limb on 27 January 2012 observed by Hinode/EIS and found that the hot (∼30MK) fast (> 500 km s-1) component was located above the flare loop by imaging spectroscopic observation. At the same time and location we also found downward flowing loops (apparent speed ∼350 km s-1) by using SDO/AIA observation. This is the first imaging spectroscopic evidence that the magnetic reconnection take place above the flare loop.