The evolution of twisting coronal magnetic flux tubes

By Tibor Török, B. Kliem. 2003

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View Paper: https://www.semanticscholar.org/paper/38fea49d21a80e65fe143c1554ab8fd50ee0450a

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In Astronomy and Astrophysics

Citations in the corpus

Interplanetary flux rope ejected from an X-ray bright point. The smallest magnetic cloud source-region ever observed (2005, background): “…statistically ambiguous (Canfield et al. 1999; Glover et al. 2000), it has been suggested that the magnetic helicity content in S-shaped magnetic configurations may reach a threshold leading to instability and eruption (van Driel-Gesztelyi et al. 2000; Török & Kliem 2003 and references therein).”
COEXISTING FLUX ROPE AND DIPPED ARCADE SECTIONS ALONG ONE SOLAR FILAMENT (2010, methodology): “Furthermore, using the theoretical coronal flux rope models by Titov & Démoulin (1999) and Török & Kliem (2003), it has been recently shown that NLFFF extrapolation codes are capable of reconstructing significantly twisted flux ropes, as well as topological features of active region magnetic…”
OBSERVING FLUX ROPE FORMATION DURING THE IMPULSIVE PHASE OF A SOLAR ERUPTION (2011, background): “Török & Kliem (2003, 2005) and Kliem & Török (2006) studied the instability of the flux rope and proposed that the kink and/or torus instability can trigger the CME.”
A MODEL FOR MAGNETICALLY COUPLED SYMPATHETIC ERUPTIONS (2011, unknown): “For further numerical details we refer to Török & Kliem (2003).”
Nonlinear Force-free Field Modeling of a Solar Active Region around the Time of a Major Flare and Coronal Mass Ejection (2007, background): “Then there are ‘‘twisted’’ flux ropes that may either emerge as such (e.g., Fan & Gibson 2004; Amari et al. 2004) or form from photospheric vortical motions (e.g., Amari et al. 1996; Török & Kliem 2003; Aulanier et al. 2005).”
Confined and Ejective Eruptions of Kink-unstable Flux Ropes (2005, methodology): “In order to avoid this problem, we replaced the line current by a pair of subphotospheric dipoles (as used in To¨rök & Kliem 2003).”
Solar filament eruptions and their physical role in triggering Coronal Mass Ejections (2012, methodology): “Using the theoretical coronal flux rope models by Titov and Démoulin (1999) and Török and Kliem (2003), it has been shown that NLFFF extrapolation codes are capable of reconstructing significantly twisted flux ropes, as well as topological features of AR magnetic fields (Valori et al., 2005,…”
Ideal kink instability of a magnetic loop equilibrium (2003, methodology): “A small amount of artificial spatial smoothing, 1−σρ = 1−σu = 0.005, is applied to the variablesρ and u, respectively, to stabilize the scheme in addition to the stabilization by the viscosity (ν = 0.05); see Török & Kliem (2003) for a detailed description of the numerical tools.”
Formation of current sheets and sigmoidal structure by the kink instability of a magnetic loop (2003, background): “See Török & Kliem (2003) for an alternative interpretation of long-lived sigmoids as loops of enhanced current density but subcritical twist.”
The Physical Processes of CME/ICME Evolution (2017, background): “…1991), the structure starts to accelerate, driven by some form of ideal MHD instabilities such as the kink or torus modes (e.g., and references therein Török and Kliem 2003, 2005; Kliem et al. 2004; Kliem and Török 2006; Démoulin and Aulanier 2010; Olmedo and Zhang 2010; Török et al. 2010).”
Coronal prominence structure and dynamics: A magnetic flux rope interpretation (2006, background): “in which an initially untwisted coronal flux tube is sheared at its footpoints have led to a loosely wound (less than two full turns) flux rope in equilibrium [Toeroek and Kliem, 2003] or, alternatively, to more tightly wound flux ropes”
The Interaction of Successive Coronal Mass Ejections: A Review (2016, methodology): “The simulation by Török et al. (2011) was established on a set of zero-β compressible ideal MHD equations (Török and Kliem, 2003) in which four flux ropes (Titov and Démoulin, 1999) were inserted with two of them under a pseudo-streamer and the other two placed on each side of the…”
Current sheet formation in quasi-separatrix layers and hyperbolic flux tubes (2005, unknown): “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).”
CRITERIA FOR FLUX ROPE ERUPTION: NON-EQUILIBRIUM VERSUS TORUS INSTABILITY (2010, background): “Return currents are indeed present in MHD simulations, but when a significant magnetic field component is present along the PIL, the direct current has a larger magnitude than the return current (Török & Kliem 2003; Aulanier et al. 2005).”