Dynamical Formation and Stability of Helical Prominence Magnetic Fields

By C. R. DeVore, S. Antiochos, E. O. Hulburt. 2000

192 citations recorded by the source corpus.

Subfields: Astronomy and Astrophysics, Molecular Biology

View Paper: https://www.semanticscholar.org/paper/e1556b40394d830bea58f56f5f01a0d2a5653102

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Citations in the corpus

Emergence of a Helical Flux Rope under an Active Region Prominence (2008, background): “…Low & Hundhausen 1995; Low 1996; Lites 2005; Zhang & Low 2005) and sheared-arcade models (e.g., Pneuman 1983; van Ballegooijen & Martens 1989, 1990; Antiochos et al. 1994; DeVore & Antiochos 2000; Martens & Zwaan 2001; Aulanier et al. 2002; Karpen et al. 2003; Mackay & van Ballegooijen 2005, 2006).”
Injection of Magnetic Energy and Magnetic Helicity into the Solar Atmosphere by an Emerging Magnetic Flux Tube (2003, background): “The evolution of the axis field line has been shown to be important in the formation of prominences within sheared coronal field distributed over the neutral line (DeVore & Antiochos 2000).”
The standard flare model in three dimensions - I. Strong-to-weak shear transition in post-flare loops (2012, background): “The relatively weak and concentrated twist in pre-eruptive field a-priori makes it hard to distinguish from a mere sheared arcade (as modeled e.g. in DeVore & Antiochos 2000; Aulanier et al. 2002), but a topological analysis clearly shows that the pre-eruptive field comprises a twisted flux rope…”
Homologous Confined Filament Eruptions via Magnetic Breakout (2008, background): “…observed similar reconnection events, between the strongly sheared filament field lines and their innermost overlying unsheared arcade lines, in our studies of filament formation, interaction, and merging in rectilinear geometries (DeVore & Antiochos 2000; DeVore et al. 2005; Aulanier et al. 2006).”
Current sheet formation in quasi-separatrix layers and hyperbolic flux tubes (2005, background): “This behavior is typical of every MHD simulation with slow line-tied boundary motions (e.g. DeVore & Antiochos 2000; Török & Kliem 2003; Aulanier et al. 2005).”
Are Magnetic Dips Necessary for Prominence Formation? (2001, background): “Note that dips are not only possible but, in fact, are very likely to form in a sheared three-dimensional field surrounding a neutral line (Antiochos et al. 1994; Devore & Antiochos 2000).”
Physics of Solar Prominences: II—Magnetic Structure and Dynamics (2010, methodology): “An alternative method of forming a similar magnetic structure was proposed by DeVore and Antiochos (2000) using a single bipolar configuration (also see Antiochos et al., 1994).”
The Formation of a Prominence in Active Region NOAA 8668. I. SOHO/MDI Observations of Magnetic Field Evolution (2001, unknown): “The contours are the Ñux density levels of ^20 and 400 G. as inputs to theoretical models of Ðlament formation (e.g., Choe & Lee 1992 ; DeVore & Antiochos 2000) but has hardly been reported from observations, possibly because of the very limited availability of high-quality magnetogram data with a…”