most citedCatastrophe versus instability for the eruption of a toroidal solar magnetic flux rope

110 citations · 356 across the 8 of their papers we have counts for

collaborators

8 papers

astro-ph.SR201663 cited

Flux-Rope Twist in Eruptive Flares and CMEs: due to Zipper and Main-Phase Reconnection

Eric Priest, Dana Longcope

The nature of three-dimensional reconnection when a twisted flux tube erupts during an eruptive flare or coronal mass ejection is considered. The reconnection has two phases: first…

astro-ph.SR201615 cited

Imaging Observations of Magnetic Reconnection in a Solar Eruptive Flare

Y. Li, X. Sun, M. D. Ding +2

Solar flares are one of the most energetic events in the solar atmosphere. It is widely accepted that flares are powered by magnetic reconnection in the corona. An eruptive flare i…

astro-ph.SR201649 cited

The formation of an inverse S-shaped active-region filament driven by sunspot motion and magnetic reconnection

X. L. Yan, E. R. Priest, Q. L. Guo +3

We present a detailed study of the formation of an inverse S-shaped filament prior to its eruption in active region NOAA 11884 from October 31 to November 2, 2013. In the initial s…

astro-ph.SR201649 cited

3D MHD modeling of twisted coronal loops

F. Reale, S. Orlando, M. Guarrasi +4

We perform MHD modeling of a single bright coronal loop to include the interaction with a non-uniform magnetic field. The field is stressed by random footpoint rotation in the cent…

astro-ph.SR201410 cited

The nature of separator current layers in MHS equilibria I. Current parallel to the separator

J. E. H. Stevenson, C. E. Parnell, E. R. Priest +1

Separators, which are in many ways the three-dimensional equivalent to two-dimensional nulls, are important sites for magnetic reconnection. Magnetic reconnection occurs in strong…

astro-ph.SR201454 cited

The Solar Cycle Variation of Topological Structures in the Global Solar Corona

Sarah J. Platten, Clare E. Parnell, Andrew L. Haynes +2

The distribution of magnetic flux across the solar photosphere results in a complex web of coronal magnetic field structures. To understand this complexity, the magnetic skeleton o…