The Emergence of a Twisted Magnetic Flux Tube into a Preexisting Coronal Arcade

By Yuhong Fan, Sarah Gibson. 2003

198 citations recorded by the source corpus.

Subfields: Astronomy and Astrophysics, Molecular Biology

View Paper: https://www.semanticscholar.org/paper/19296dc0974e2aad35a8501e6e6fc39c707fd8f4

How researchers see this paper

The researchers whose trusted networks rank it highest, strongest advocate first. Every researcher gets a different order.

In Astronomy and Astrophysics

1. Yuhong Fan
2. P. Démoulin
3. S. Gibson
4. C. Schrijver
5. G. Aulanier
6. Tibor Török
7. T. Wiegelmann
8. G. Barnes

In Molecular Biology

1. Yuhong Fan
2. S. Gibson
3. P. Démoulin
4. Tibor Török
5. B. Kliem
6. Matthias Rempel
7. Yang Liu
8. Mark C. M. Cheung

Citations in the corpus

• Topological Methods for the Analysis of Solar Magnetic Fields (2005, background): “Numerical simulations (Fan and Gibson 2003) have confirmed that free dynamical evolution leads to current sheets along the BP surfaces in fields of the Titov and Deḿoulin type.”
• The Calm before the Storm: The Link between Quiescent Cavities and Coronal Mass Ejections (2006, background): “…Rust 1994; Rust & Kumar 1994; Lites & Low 1997; Gibson & Low 1998; Aulanier & Démoulin 1998), X-ray sigmoids (Rust & Kumar 1994; Titov & Démoulin 1999; Low & Berger 2003; Fan & Gibson 2003, 2004; Kliem et al. 2004; Gibson et al. 2004), and three-part CMEs and magnetic clouds, as referenced above.”
• Coronal Mass Ejections as Loss of Confinement of Kinked Magnetic Flux Ropes (2005, background): “Fan & Gibson (2003, 2004), Kliem et al. (2004), and Gibson et al. (2004) have discussed in detail how the current sheet forms and its close relation to the baldpatch separatrix surface that separates the twisted field lines that graze the photosphere and the neighboring anchored field lines (Titov…”
• An Overview of Existing Algorithms for Resolving the 180° Ambiguity in Vector Magnetic Fields: Quantitative Tests with Synthetic Data (2006, methodology): “Case #1: Twisted Fluxrope in a Potential-Field Arcade, µ = 1.0 The first test case is a “photospheric” vector magnetogram constructed from the MHD model of Fan and Gibson (Fan and Gibson (2003); Fan and Gibson (2004)), paper.tex; 25/05/2006; 9:44; p.15 provided courtesy of Y. Fan.”
• The Partial Expulsion of a Magnetic Flux Rope (2006, background): “…a pre-CME flux rope (Wolfson et al. 1987; Low & Hundhausen 1995; Linker et al. 2003; Gibson et al. 2006), as are transient sigmoid brightenings (Rust & Kumar 1996; Fan & Gibson 2003, 2004; Kliem et al. 2004) and their transition to cusped postflare loops (Amari et al. 2003b; To¨rök & Kliem 2005).”
• Coronal Mass Ejections: Observations (2012, background): “Recent models describing the onset and early evolution of CMEs (e.g., Moore and Roumeliotis, 1992; Antiochos et al., 1999; Fan and Gibson, 2003; Lynch et al., 2005) provide a variety of mechanisms by which this may be accomplished.”
• Confined and Ejective Eruptions of Kink-unstable Flux Ropes (2005, background): “They have shown that this model relaxes to a numerical equilibrium very close to the analytical expressions in the case of subcritical twist and that the helical kink instability develops for supercritical twist (see also Fan & Gibson 2003, 2004).”
• Eruption of a Buoyantly Emerging Magnetic Flux Rope (2003, background): “In the case of Fan & Gibson (2003), a sigmoid-shaped current sheet forms where an emerging kink-unstable flux rope folds back onto itself.”
• Eruption of a Kink-unstable Filament in NOAA Active Region 10696 (2005, unknown): “In coronal applications of curved and line-tied flux-rope models, this deformation results in an exponentially growing height of the flux rope’s apex in the linear phase of the instability, as shown in numerical simulations (Fan & Gibson 2003; Török, Kliem, & Titov 2004).”
• Generalized Squashing Factors for Covariant Description of Magnetic Connectivity in the Solar Corona (2007, background): “This seems to be valid at least for the third topological phase of the flux rope emergence, while an additional interaction with the photosphere must be involved at the first and second topological phases, where the BPs are present (Titov & Démoulin 1999; Fan & Gibson 2003).”
• Interplanetary flux rope ejected from an X-ray bright point. The smallest magnetic cloud source-region ever observed (2005, methodology): “The results of these topological studies are supported by the recent numerical simulations of Fan & Gibson (2003), Gibson et al. (2004) and Kliem et al. (2004).”
• OBSERVING FLUX ROPE FORMATION DURING THE IMPULSIVE PHASE OF A SOLAR ERUPTION (2011, background): “Considerable efforts have also been made in numerical MHD simulations to study the formation and dynamic behavior of flux ropes (Amari et al. 2000, 2003; Aulanier et al. 2010; Fan & Gibson 2003, 2004).”
• SIMULATION OF THE FORMATION OF A SOLAR ACTIVE REGION (2010, methodology): “Following Fan & Gibson (2003), the magnetic field distribution of the flux tube in a spherical coordinate system with the torus centered at the origin is given by ~B = ∇× [A(r, θ) r sin θ φ̂] +Bφ(r, θ)φ̂, (1) A = 1 2 λaBt exp (−ω2/a2), and (2) Bφ = (r sin θ) −1aBt exp (−ω2/a2).”