EUV spectral lines and the nanoflare model of coronal heating

M. LÓPEZ FUENTES; JAMES KLIMCHUK

San Juan

Conferencia; Towards Future Research on Space Weather Drivers; 2019

The mechanism of coronal heating by nanoflares has been proposed to explain a diversity of coronal observations. The theory is based on the idea that coronal loops are formed by unresolved elementary magnetic strands that are stressed by photospheric motions, generating conditions for magnetic reconnection and consequent plasma heating. It is expected that this heating process also produce conspicuous plasma flows along individual strands. We explore some observational consequences of these flows, particularly, their effect on EUV spectral lines, such as broadenings and Doppler shifts. In order to simulate the evolution of a large number of heated strands, in previous works (see e.g., Lopez-Fuentes and Klimchuk, 2016, ApJ, 828, 86) we used the 0D model \"Enthalpy Based Thermal Evolution of Loops\" (EBTEL, Cargill et al., 2012, ApJ, 752, 161), which is much less demanding numerically than more sophisticated full hydrodynamic models. In this work, we compare the results obtained with this model and with a 1D hydrodynamic code (HYDRAD, Bradshaw et al., 2012, ApJ, 758, 53), by analysing the effect that they have on synthetic spectral lines constructed from the emission produced by individual nanoflares.