Investigating Alfven Wave Turbulence in Chromosphere and Corona Using Extreme Ultraviolet Imaging Spectrometer (EIS)

Friday, 19 December 2014: 3:06 PM
Mahboubeh Asgari-Targhi, Harvard-Smithsonian Center for Astrophysics, Cambridge, MA, United States, Shinsuke Imada, Nagoya University, Solar-Terrestrial Environment Laboratory, Nagoya, Japan and Edward E DeLuca, SAO, Cambridge, MA, United States
The solar corona is known to be very dynamic. Mass motions due to Alfven wave turbulence are one of the main causes of plasma flows within the coronal loops. Using observations from EIS we analyze the structure of active region loops observed on 2012 September 7. We study the spectral line profiles of Fe XII, Fe XIII, Fe XV and Fe XVI and compare the non-thermal line broadening from this region to line-of-sight velocity from our Alfven wave turbulence modeling of the loops. In our computations, the relationship between the width of the coronal emission lines and the orientation of the coronal loops with respect to the line-of-sight direction is taken in to account. We predict that in coronal loops, the transverse component of plasma flows with respect to the loop axis move at the speed of 15–40 km/s. In conclusion, Alfven waves are a strong candidate in explaining the flows within the coronal loops and play an important role in the heating of the chromosphere and corona.