This article has an erratum: [https://doi.org/10.1051/0004-6361/202038925e]
Volume 644, December 2020
|Number of page(s)||7|
|Section||The Sun and the Heliosphere|
|Published online||25 November 2020|
Exploring the coronal evolution of AR 12473 using time-dependent, data-driven magnetofrictional modelling⋆
Department of Physics, University of Helsinki, Helsinki, Finland
Accepted: 2 October 2020
Aims. We present a detailed examination of the magnetic evolution of AR 12473 using time-dependent, data-driven magnetofrictional modelling.
Methods. We used maps of the photospheric electric field inverted from vector magnetogram observations, obtained by the Helioseismic and Magnetic Imager onboard the Solar Dynamics Observatory (SDO), to drive our fully time-dependent, data-driven magnetofrictional model. Our modelled field was directly compared to extreme ultraviolet observations from the Atmospheric Imaging Assembly, also onboard SDO. Metrics were also computed to provide a quantitative analysis of the evolution of the magnetic field.
Results. The flux rope associated with the eruption on 28 December 2015 from AR 12473 was reproduced by the simulation and found to have erupted due to a torus instability.
Key words: Sun: coronal mass ejections (CMEs) / Sun: corona / magnetic fields / magnetic reconnection / methods: numerical / methods: data analysis
Movies associated with Figs. 1 and 5 are available at https://www.aanda.org
© ESO 2020
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