Observations and Modeling of a Filament on the Sun

By A. A. Ballegooijen. 2004

243 citations recorded by the source corpus.

View Paper: https://www.semanticscholar.org/paper/6254b7a57f9b9b6d30fd6e3104fc9fc819f5b745

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In Astronomy and Astrophysics

Citations in the corpus

Physics of Solar Prominences: II—Magnetic Structure and Dynamics (2010, methodology): “Furthermore, the case of identical chiralities and aligned axial fields successfully reproduces the observations of filament merging (e.g., Martin et al., 1994; Rust, 2001; Schmieder et al., 2004; van Ballegooijen, 2004).”
Coronal prominence structure and dynamics: A magnetic flux rope interpretation (2006, methodology): “Observed filament properties such as the orientation of filament threads relative to underlying magnetic field (e.g., filament chirality), and ‘‘barbs’’ protruding from the side of the filament [Martin, 1998] have been explained in terms of idealized flux rope models [Rust and Kumar, 1994; Low and H”
Solar filament eruptions and their physical role in triggering Coronal Mass Ejections (2012, methodology): “Figure 4 shows two examples where flux rope have been evidenced using NLFFF extrapolations. van Ballegooijen (2004) proposed another method by inserting a flux rope in the magnetic region and led the system to relax using a magneto-frictionnal method.”
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).”
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).”
The Partial Expulsion of a Magnetic Flux Rope (2006, background): “…OF PARTIALLY EXPELLED FLUX ROPES It is well known that filaments often re-form after eruptions as active regions evolve: one possible explanation is flux rope re-formation due to turbulent boundary flux diffusion as active regions gradually disperse (Amari et al. 2003b; van Ballegooijen 2004).”