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3D rMHD Simulation of a small C-class flare; from convection zone to corona

Presentation #106.41 in the session Solar Eruptive Events: Posters.

Published onSep 18, 2023
3D rMHD Simulation of a small C-class flare; from convection zone to corona

Our ability to predict the occurrence and impact of flares is hampered by an incomplete picture of underlying physical drivers, triggers, and instabilities. This situation is being ameliorated by recent advances in the gathering of both high cadence, high resolution data as well as long term evolutionary data, spanning the solar atmosphere from the photosphere to corona with ground based and space borne instruments such as DKIST and the SST, IRIS, SDO/AIA, Hinode/EIS and SOT, SOLO/EUI and PHI, and SDO/HMI. The situation should become even better with the launches of MUSE and Solar C/EUVST. However, flares are complicated phenomena, and making sense of them can be greatly helped with the assistance given by 3D rMHD simulations spanning a similar range of the solar atmosphere. We present a Bifrost simulation featuring magnetic flux emergence with amplitude approximately that found in a mid sized active region. After several hours solar time the simulation produces a C-class flare. We synthisize several observables relevant to IRIS, Hinode, AIA, and future MUSE observations and compare these to and observed flare of the same class. Similarities and differences between the observed and syntesized data and their physical interpretation and consequences are discussed.

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