Modeling Nanoflare Heating of AR11726 Observed by EUNIS and EIS

Abstract:

High-spatial and spectral resolution observations of coronal active regions (AR) in the extreme -ultraviolet (EUV) suggest that the solar corona is a non-uniform environment structured into bundles of magnetic loops heated to temperatures exceeding 5 MK. Here we present results from a parameter study modeling the EUV emission produced in AR11726 using an impulsive nanoflare heating model. We have used HMI vector magnetograms to estimate the coronal magnetic field and traced closed field regions within the AR to obtain more than 30,000 individual flux tubes. We have simulated nanoflares within each of these using a 1D hydrodynamic loop. We have varied the energy released by nanoflares as a function of magnetic field strength, loop length, flare duration and frequency. We compare the simulated emission with multiple hihg-temperature lines observed by the EUNIS and Hinode/EIS instruments to constrain the heating parameters.