Comparative Study of Data-driven Solar Coronal Field Models Using a Flux Emergence Simulation as a Ground-truth Data Set

• Published in: The Astrophysical journal 2020-02, Vol.890 (2), p.103
• Main Authors: Toriumi, Shin, Takasao, Shinsuke, Cheung, Mark C. M., Jiang, Chaowei, Guo, Yang, Hayashi, Keiji, Inoue, Satoshi
• Format: Article
• Language: English
• Subjects: Algorithms; Astrophysics; Atmospheric models; Comparative studies; Computer simulation; Constraint modelling; Corona; Coronal mass ejection; Datasets; Emergence; Fluctuations; Helicity; Magnetic fields; Magnetic flux; Magnetohydrodynamics; Photosphere; Qualitative analysis; Solar active regions; Solar corona; Solar coronal mass ejections; Solar flares; Solar magnetic field; Solar magnetic fields; Solar magnetic flux emergence; Solar photosphere; Spatial resolution; Toruses; Velocity distribution
• ISSN: 0004-637X; 1538-4357
• DOI: 10.3847/1538-4357/ab6b1f

For a better understanding of the magnetic field in the solar corona and dynamic activities such as flares and coronal mass ejections, it is crucial to measure the time-evolving coronal field and accurately estimate the magnetic energy. Recently, a new modeling technique called the data-driven coronal field model, in which the time evolution of magnetic field is driven by a sequence of photospheric magnetic and velocity field maps, has been developed and revealed the dynamics of flare-productive active regions. Here we report on the first qualitative and quantitative assessment of different data-driven models using a magnetic flux emergence simulation as a ground-truth (GT) data set. We compare the GT field with those reconstructed from the GT photospheric field by four data-driven algorithms. It is found that, at minimum, the flux rope structure is reproduced in all coronal field models. Quantitatively, however, the results show a certain degree of model dependence. In most cases, the magnetic energies and relative magnetic helicity are comparable to or at most twice of the GT values. The reproduced flux ropes have a sigmoidal shape (consistent with GT) of various sizes, a vertically standing magnetic torus, or a packed structure. The observed discrepancies can be attributed to the highly non-force-free input photospheric field, from which the coronal field is reconstructed, and to the modeling constraints such as the treatment of background atmosphere, the bottom boundary setting, and the spatial resolution.