Time-dependent Data-driven Modeling of Active Region Evolution Using Energy-optimized Photospheric Electric Fields

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http://hdl.handle.net/10138/301503

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Pomoell , J , Lumme , E & Kilpua , E 2019 , ' Time-dependent Data-driven Modeling of Active Region Evolution Using Energy-optimized Photospheric Electric Fields ' , Solar Physics , vol. 294 , no. 4 , 41 . https://doi.org/10.1007/s11207-019-1430-x

Titel: Time-dependent Data-driven Modeling of Active Region Evolution Using Energy-optimized Photospheric Electric Fields
Författare: Pomoell, Jens; Lumme, Erkka; Kilpua, Emilia
Medarbetare: University of Helsinki, Department of Physics
University of Helsinki, Department of Physics
University of Helsinki, Department of Physics
Datum: 2019-04
Språk: eng
Sidantal: 28
Tillhör serie: Solar Physics
ISSN: 0038-0938
Permanenta länken (URI): http://hdl.handle.net/10138/301503
Abstrakt: In this work, we present results of a time-dependent data-driven numerical simulation developed to study the dynamics of coronal active region magnetic fields. The evolving boundary condition driving the model, the photospheric electric field, is inverted using a time sequence of vector magnetograms as input. We invert three distinct electric field datasets for a single active region. All three electric fields reproduce the observed evolution of the normal component of the magnetic field. Two of the datasets are constructed so as to match the energy input into the corona to that provided by a reference estimate. Using the three inversions as input to a time-dependent magnetofrictional model, we study the response of the coronal magnetic field to the driving electric fields. The simulations reveal the magnetic field evolution to be sensitive to the input electric field despite the normal component of the magnetic field evolving identically and the total energy injection being largely similar. Thus, we demonstrate that the total energy injection is not sufficient to characterize the evolution of the coronal magnetic field: coronal evolution can be very different despite similar energy injections. We find the relative helicity to be an important additional metric that allows one to distinguish the simulations. In particular, the simulation with the highest relative helicity content produces a coronal flux rope that subsequently erupts, largely in agreement with extreme-ultraviolet imaging observations of the corresponding event. Our results suggest that time-dependent data-driven simulations that employ carefully constructed driving boundary conditions offer a valuable tool for modeling and characterizing the evolution of coronal magnetic fields.
Subject: Helicity: magnetic
Magnetic fields: corona
Corona: active
Corona: models
Magnetic fields: photosphere
CORONAL MASS EJECTIONS
VECTOR MAGNETOGRAMS
115 Astronomy, Space science
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