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Twisted versus braided magnetic flux ropes in coronal geometry. I. Construction and relaxation

Prior, C.; Yeates, A.

Twisted versus braided magnetic flux ropes in coronal geometry. I. Construction and relaxation Thumbnail


Authors

A. Yeates



Abstract

We introduce a technique for generating tubular magnetic fields with arbitrary axial geometry and internal topology. As an initial application, this technique is used to construct two magnetic flux ropes that have the same sigmoidal tubular shape, but have different internal structures. One is twisted, the other has a more complex braided magnetic field. The flux ropes are embedded above the photospheric neutral line in a quadrupolar linear force-free background. Using resistive-magnetohydrodynamic simulations, we show that both fields can relax to stable force-free equilibria whilst maintaining their tubular structure. Both end states are nonlinear force-free; the twisted field contains a single sign of alpha (the force-free parameter), indicating a twisted flux rope of a single dominant chirality, the braided field contains both signs of alpha, indicating a flux rope whose internal twisting has both positive and negative chirality. The electric current structures in these final states differ significantly between the braided field, which has a diffuse structure, and the twisted field, which displays a clear sigmoid. This difference might be observable.

Citation

Prior, C., & Yeates, A. (2016). Twisted versus braided magnetic flux ropes in coronal geometry. I. Construction and relaxation. Astronomy & Astrophysics, 587, Article A125. https://doi.org/10.1051/0004-6361/201527231

Journal Article Type Article
Acceptance Date Nov 21, 2015
Online Publication Date Mar 2, 2016
Publication Date Mar 1, 2016
Deposit Date Mar 3, 2016
Publicly Available Date Mar 28, 2024
Journal Astronomy and astrophysics.
Print ISSN 0004-6361
Electronic ISSN 1432-0746
Publisher EDP Sciences
Peer Reviewed Peer Reviewed
Volume 587
Article Number A125
DOI https://doi.org/10.1051/0004-6361/201527231

Files

Accepted Journal Article (10.5 Mb)
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Copyright Statement
Reproduced with permission from Astronomy & Astrophysics, © ESO






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