Onset of Coronal Mass Ejections Due to Loss of Confinement of Coronal Flux Ropes

By Yuhong Fan, S. Gibson. 2007

285 citations recorded by the source corpus.

Subfields: Astronomy and Astrophysics, Molecular Biology

View Paper: https://www.semanticscholar.org/paper/b6d43061f878ef5294fc18307310114b7bb28f59

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Citations in the corpus

DIFFERENTIAL EMISSION MEASURE ANALYSIS OF MULTIPLE STRUCTURAL COMPONENTS OF CORONAL MASS EJECTIONS IN THE INNER CORONA (2012, methodology): “…the hot channel plays in the eruption process appears similar to that of flux ropes in the modeling and simulations of CMEs (e.g., Chen 1996; Chen & Shibata 2000; Lin & Forbes 2000; Török & Kliem 2005; Kliem & Török 2006; Aulanier et al. 2010; Fan & Gibson 2007; Fan 2010; Olmedo & Zhang 2010).”
Solar filament eruptions and their physical role in triggering Coronal Mass Ejections (2012, background): “Then, many models start with the formation of a flux rope and bring it to an unstable state (Amari et al., 2000; Lin et al., 2001; Amari et al., 2005; Forbes et al., 2006; Fan and Gibson, 2007; Aulanier et al., 2010; Olmedo and Zhang, 2010; Zuccarello et al., 2012).”
MAGNETIC FIELD STRUCTURES TRIGGERING SOLAR FLARES AND CORONAL MASS EJECTIONS (2012, background): “…topologies (Antiochos et al. 1999; Sterling & Moore 2004; Williams et al. 2005), flux rope (Forbes & Priest 1995; Török & Kliem 2005; Chen 1996; Fan & Gibson 2007), narrow magnetic lanes between major sunspots (Zirin & Wang 1993; Kubo et al. 2007), topological complexity (Schmieder et al.…”
Driving major solar flares and eruptions: A review (2008, background): “Kliem and Török (2006) (also, e.g., Fan and Gibson 2007) discuss the torus instability, and find a critical field gradient beyond which the configuration is unstable.”
The Interaction of Successive Coronal Mass Ejections: A Review (2016, background): “…an ideal process, due to some instabilities, e.g. the kink instability (see, e.g., Hood and Priest, 1979, 1980), torus instability (see, e.g., Török, Kliem, and Titov, 2004, Kliem and Török, 2006, Fan and Gibson, 2007) and catastrophe (Forbes and Priest, 1995; Lin and Forbes, 2000; Hu, 2001).”
COEXISTING FLUX ROPE AND DIPPED ARCADE SECTIONS ALONG ONE SOLAR FILAMENT (2010, background): “…CME models require the presence of a flux rope prior to, or at the onset of, an eruption (e.g., Forbes & Isenberg 1991; Török & Kliem 2005; Fan & Gibson 2007), whereas others assume that the preeruptive configuration is that of an arcade, and that a flux rope is formed later on, during…”
CRITERIA FOR FLUX ROPE ERUPTION: NON-EQUILIBRIUM VERSUS TORUS INSTABILITY (2010, background): “The two last phases are the most spectacular ones, so they are better constrained by observations and they are more deeply modeled, in particular with MHD simulations (e.g. Amari et al. 2003; Fan & Gibson 2007; Török & Kliem 2007).”
A MODEL FOR MAGNETICALLY COUPLED SYMPATHETIC ERUPTIONS (2011, background): “The slow rise lasts until the rope reaches the critical height for TI onset at t ≈ 40 τa, after which it rapidly accelerates upward driven by the instability (Török & Kliem 2007; Fan & Gibson 2007; Schrijver et al. 2008; Aulanier et al. 2010).”