Speaker
Description
Magnetic reconnection is a ubiquitous process in the solar atmosphere. During reconnection, the topology of magnetic field lines changes and magnetic energy is transferred to plasma kinetic, thermal, or non-thermal energy. It is believed that magnetic reconnection is an underlying mechanism that powers various energetic phenomena in the solar atmosphere. However, numerical modeling of magnetic reconnection is computationally expensive even for local solar atmospheric modeling. Aiming at global MHD modeling of the solar atmosphere and space weather applications, we experiment with data-driven model order reduction methods, including proper orthogonal decomposition (POD) and dynamic mode decomposition (DMD), to generate data sets that are able to recover the detailed process of magnetic reconnection and are also computationally affordable. While already being able to accurately recover fundamental quantities in the magnetic reconnection process, including temperature, velocity, etc., it is important to further examine, for example, EUV observables, energization of non-thermal particles. Therefore, we will correspondingly discuss the potential of the reduced order models.
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