Mean Field Model for the Formation of Filament Channels on the Sun

By A. A. Ballegooijen, E. Priest, D. H. Mackay. 2000

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In Astronomy and Astrophysics

Citations in the corpus

Models of the Large-Scale Corona. I. Formation, Evolution, and Liftoff of Magnetic Flux Ropes (2006, methodology): “In order to follow the evolution on long time scales, the coronal plasma velocity is assumed to be proportional to the Lorentz force (magnetofriction), causing the coronal field to evolve through a series of non-linear force-free states (van Ballegooijen et al. 2000).”
Origin and Evolution of Filament-Prominence Systems (2001, methodology): “Finally, we will brieÑy analyze two recent and impressive full-disk numerical simulations of the formation and evolution of Ðlament channels and Ðlaments by van Ballegooijen et al. (1998) and van Ballegooijen et al. (2000).”
Nonlinear Force-Free Modeling of Coronal Magnetic Fields. II. Modeling a Filament Arcade and Simulated Chromospheric and Photospheric Vector Fields (2008, methodology): “The procedure and the boundary conditions were described in detail by van Ballegooijen (2004) and van Ballegooijen et al. (2007), while the magnetofrictional code used to relax the field to an essentially force-free state was described by van Ballegooijen, Priest, and Mackay (2000).”
The Role of Magnetic Reconnection in the Observable Features of Solar Eruptions (2004, background): “…in a sheared magnetic arcade (van Ballegooijen & Martens 1989; Choe & Lee 1992; Inhester et al. 1992; Amari et al. 2000; Aulanier et al. 2000; van Ballegooijen et al. 2000; Mackay & van Ballegooijen 2001), or it can directly emerge from the convective zone into the corona (see Lites et al. 1995;…”
Coronal prominence structure and dynamics: A magnetic flux rope interpretation (2006, background): “Another possibility is flux rope formation as a result of a more gradual diffusion of decaying active region flux on the photosphere [van Ballegooijen et al., 1998, 2000; Mackay and van Ballegooijen, 2001, 2005, 2006; Amari et al., 2003a].”
COEXISTING FLUX ROPE AND DIPPED ARCADE SECTIONS ALONG ONE SOLAR FILAMENT (2010, methodology): “…the extrapolation domain (Wheatland et al. 2000), and it is 5.0 × 10−4 for the extrapolation of preprocessed and smoothed photospheric data generated by the flux rope insertion method (van Ballegooijen et al. 2000; van Ballegooijen 2004), using the optimization method (Metcalf et al. 2008).”
Physics of Solar Prominences: II—Magnetic Structure and Dynamics (2010, unknown): “In force-free field models (e.g., Aulanier and Démoulin, 1998; Mackay, Longbottom & Priest, 1999; van Ballegooijen et al., 2000; Mackay and van Ballegooijen, 2005) this chirality is directly related to the dominant sign of magnetic helicity that is contained within the filament and filament…”