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qiang hu   Submitted: 2006-11-22 15:28

We develop an approach to deriving three-dimensional non-force free coronal magnetic field from vector magnetograms. Based on the principle of Minimum Dissipation Rate, a general non-force free magnetic field is expressed as superposition of one potential field, and two constant-α (linear) force free fields. Each is extrapolated from their bottom boundary data, providing the normal component only. The constant α parameters are distinct, and determined by minimizing the deviations between the numerically computed and measured transverse magnetic field at the bottom boundary. The boundary conditions required are at least two layers of vector magnetograms, one at the photospheric level and the other the chromospheric level, presumably. We apply it to a few analytic test cases, especially to two non-linear force free cases examined by Schrijver et al. (2006). We find that for one case with small α parameters, the quantitative measures of the quality of our result are better than the median values of those from a set of non-linear force free methods. The reconstructed magnetic field configuration is valid up to a vertical height of the transverse scale. For the other cases, the results remain valid to a lower vertical height due to the limitations of the linear force free field solver. As based on the Fast Fourier Transform algorithm, our method is much faster and easy to implement. We discuss the potential usefulness of our method and its limitations.


Publication Status: Solar Physics (submitted; under revision)
Last Modified: 2006-12-01 12:06
Go to main E-Print page  MHD seismology of coronal loops using the period and damping of quasi-mode kink oscillations  A Multiple flare scenario where the classic long duration flare was not the source of a CME  Edit Entry  Download Preprint  Delete Entry 

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