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EP: Fachverband Extraterrestrische Physik
EP 6: Sun and Heliosphere III
EP 6.4: Vortrag
Dienstag, 1. April 2025, 17:15–17:30, ZHG101
1D hydrodynamics simulations of impulsively heated short loops to explain the origin of EUV brightenings in the quiet Sun. — •Antoine Dolliou1,2, James Klimchuk3, Susanna Parenti2, and Karine Bocchialini2 — 1Max Planck Institute for Solar System Research, Justus-von-Liebig-Weg 3, 37077 Göttingen, Germany — 2Université Paris-Saclay, CNRS, Institut d'Astrophysique Spatiale, 91405 Orsay, France — 3NASA Goddard Space Flight Center, 8800 Greenbelt Road, Greenbelt, MD 20771 USA
The Sun upper atmosphere, the corona, is maintained to more than 1 MK, through processes that are still not fully understood. One of the main theories of the coronal formation suggests that the energy is dissipated through small scales (< 1E24 erg) and impulsive processes (Parker et al., ApJ, 1988). On 2020 May 30, the High Resolution Imager EUV (HRIEUV), onboard Solar Orbiter, was used to detect small (400 to 4000 km), short lived (10 to 100 s) EUV brightenings in the quiet Sun. Their contribution to coronal heating and their physical origin is actively studied. The aim of this work is to understand their physical origin. To do so, we simulate impulsively heated short loop, using the 1D hydrodynamics code HYDRAD (Bradshaw et al., A&A, 2003). We use two types of loops with distinct thermal behavior: cool (T < 0.1 MK) and hot (T > 0.1 MK) loops. The synthetic light curves of HRIEUV, SDO/AIA and Solar Orbiter/SPICE are computed and compared with those obtained from observations. The results showed that cool loops are good candidates to explain the physical origin of EUV brightenings, contrary to most hot loops models.
Keywords: Coronal heating; 1D Hydrodynamic simulations; EUV brightenings; Short magnetic loops