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Origin and structures of solar eruptions II: Magnetic modeling

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Abstract

The topology and dynamics of the three-dimensional magnetic field in the solar atmosphere govern various solar eruptive phenomena and activities, such as flares, coronal mass ejections, and filaments/prominences. We have to observe and model the vector magnetic field to understand the structures and physical mechanisms of these solar activities. Vector magnetic fields on the photosphere are routinely observed via the polarized light, and inferred with the inversion of Stokes profiles. To analyze these vector magnetic fields, we need first to remove the 180° ambiguity of the transverse components and correct the projection effect. Then, the vector magnetic field can be served as the boundary conditions for a force-free field modeling after a proper preprocessing. The photospheric velocity field can also be derived from a time sequence of vector magnetic fields. Three-dimensional magnetic field could be derived and studied with theoretical force-free field models, numerical nonlinear force-free field models, magnetohydrostatic models, and magnetohydrodynamic models. Magnetic energy can be computed with three-dimensional magnetic field models or a time series of vector magnetic field. The magnetic topology is analyzed by pinpointing the positions of magnetic null points, bald patches, and quasi-separatrix layers. As a well conserved physical quantity, magnetic helicity can be computed with various methods, such as the finite volume method, discrete flux tube method, and helicity flux integration method. This quantity serves as a promising parameter characterizing the activity level of solar active regions.

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Acknowledgements

The authors thank Prof. Feng X S and Prof. Wan W X for the invitation to write the review paper, and thank the three anonymous referees for constructive comments that improve the paper. Guo Y, Cheng X, and Ding M D are supported by National Natural Science Foundation of China (Grant Nos. 11533005, 11203014, 11373023, and 11303016) and National Key Basic Research Special Foundation (Grant No. 2014CB744203).

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  1. School of Astronomy and Space Science, Nanjing University, Nanjing, 210023, China

    Yang Guo, Xin Cheng & MingDe Ding

  2. Key Laboratory for Modern Astronomy and Astrophysics (Nanjing University), Ministry of Education, Nanjing, 210023, China

    Yang Guo, Xin Cheng & MingDe Ding

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Guo, Y., Cheng, X. & Ding, M. Origin and structures of solar eruptions II: Magnetic modeling. Sci. China Earth Sci. 60, 1408–1439 (2017). https://doi.org/10.1007/s11430-017-9081-x

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