2018/04/16 by V. Polito, P. Testa, J. Allred +5 · 2 citations
Physics and Astronomy · #astro-ph.SR
paper · pdf · doi:10.3847/1538-4357/aab49e
published as 2018ApJ...856..178P
arxiv created 2018/04/16 · arxiv updated 2018/04/18
We present the results of 1D hydrodynamic simulations of coronal loops which are subject to nanoflares, caused by either in-situ thermal heating, or non-thermal electrons (NTE) beams. The synthesized intensity and Doppler shifts can be directly compared with IRIS and AIA observations of rapid variability in the transition region (TR) of coronal loops, associated with transient coronal heating. We find that NTE with high enough low-energy cutoff (E_\textrmC) deposit energy in the lower TR and chromosphere causing blueshifts (up to~∼~20 km/s) in the IRIS \siiv~lines, which thermal conduction cannot reproduce. The E_\textrmC threshold value for the blueshifts depends on the total energy of the events (≈~5 keV for 1024 ergs, up to 15 keV for 1025 ergs). The observed footpoint emission intensity and flows, combined with the simulations, can provide constraints on both the energy of the heating event and E_\textrmC. The response of the loop plasma to nanoflares depends crucially on the electron density: significant \siiv~intensity enhancements and flows are observed only for initially low-density loops (<~109~cm-3). This provides a possible explanation of the relative scarcity of observations of significant moss variability. While the TR response to single heating episodes can be clearly observed, the predicted coronal emission (AIA 94Å) for single strands is below current detectability, and can only be observed when several strands are heated closely in time. Finally, we show that the analysis of the IRIS \mgii~chromospheric lines can help further constrain the properties of the heating mechanisms.