On the quasi-three dimensional configuration of magnetic clouds. (arXiv:2010.11889v1 [astro-ph.SR])

On the quasi-three dimensional configuration of magnetic clouds. (arXiv:2010.11889v1 [astro-ph.SR])
<a href="http://arxiv.org/find/astro-ph/1/au:+Hu_Q/0/1/0/all/0/1">Qiang Hu</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+He_W/0/1/0/all/0/1">Wen He</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Qiu_J/0/1/0/all/0/1">Jiong Qiu</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Vourlidas_A/0/1/0/all/0/1">A. Vourlidas</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Zhu_C/0/1/0/all/0/1">Chunming Zhu</a>

We develop an optimization approach to model the magnetic field configuration
of magnetic clouds, based on a linear-force free formulation in three
dimensions. Such a solution, dubbed the Freidberg solution, is kin to the
axi-symmetric Lundquist solution, but with more general “helical symmetry”. The
merit of our approach is demonstrated via its application to two case studies
of in-situ measured magnetic clouds. Both yield results of reduced
$chi^2approx 1$. Case 1 shows a winding flux rope configuration with one
major polarity. Case 2 exhibits a double-helix configuration with two flux
bundles winding around each other and rooted on regions of mixed polarities.
This study demonstrates the three-dimensional complexity of the magnetic cloud
structures.

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