Flows in active region loops observed by Hinode EIS

Abstract

We aim to investigate the overall characteristics of coronal active region loops and their evolution. The Hinode database was searched for observations of active regions as they crossed the Sun centre. NOAA 10926 was selected. The morphology of this young active region did not significantly change over the course of a few days. Persistent redshifts, stronger in cooler lines (about 5-10 km s^-1 in Fe XII and 20-30 km s^-1 in Fe VIII), were observed in most loop structures with the EUV Imaging Spectrometer. Persistent blueshifts, stronger in the hotter lines (typically 5-20 km s^-1 in Fe XII and 10-30 km s^-1 in Fe XV), were present in areas of weak emission, in a sharp boundary between the low-lying “hot” 3 MK loops and the higher “cooler” 1 MK loops.