Abstract
We discuss the self-consistent time-dependent numerical boundary conditions on the basis of theory of characteristics for magnetohydrodynamics (MHD) simulations of solar plasma flows. The importance of using self-consistent boundary conditions is demonstrated by using an example of modeling coronal dynamic structures. This example demonstrates that the self-consistent boundary conditions assure the correctness of the numerical solutions. Otherwise, erroneous numerical solutions will appear.
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Wu, S.T., Wang, A.H. & Guo, W.P. Numerical boundary conditions for solar magnetohydrodynamic flows using the method of characteristics. Astrophys Space Sci 243, 149–153 (1996). https://doi.org/10.1007/BF00644045
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DOI: https://doi.org/10.1007/BF00644045