Eruption of a Kink-unstable Filament in NOAA Active Region 10696

By David R. Williams, Tibor Török, P. Démoulin, L. van Driel-Gesztelyi, B. Kliem. 2005

145 citations recorded by the source corpus.

We present rapid-cadence Transition Region and Coronal Explorer (TRACE) observations that show evidence of a filament eruption from NOAA active region 10696, accompanied by an X2.5 flare, on 2004 November 10. The eruptive filament, which manifests as a fast coronal mass ejection some minutes later, rises as a kinking structure with an apparently exponential growth of height within TRACE's field of view. We compare the characteristics of this filament eruption with MHD numerical simulations of a kink-unstable magnetic flux rope, finding excellent qualitative agreement. We suggest that while tether weakening by breakout-like quadrupolar reconnection may be the release mechanism for the previously confined flux rope, the driver of the expansion is most likely the MHD helical kink instability.

Subfields: Astronomy and Astrophysics

View Paper: https://www.semanticscholar.org/paper/d3ec2e5384a25f34fb1eea52f530a73db8fca86d

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In Astronomy and Astrophysics

Citations in the corpus

Eruption of magnetic flux ropes during flux emergence (2008, unknown): “In many cases, the emerging flux merely acts as a trigger for the eruption of an already existing filament (Feynman & Martin 1995; Williams et al. 2005).”
DIRECT EVIDENCE FOR A FAST CORONAL MASS EJECTION DRIVEN BY THE PRIOR FORMATION AND SUBSEQUENT DESTABILIZATION OF A MAGNETIC FLUX ROPE (2012, background): “…very viable for CMEs originating in the QS. Finally, prominences either quiescent or eruptive often exhibit helical structures, which represents a strong indication of a flux rope topology (e.g., Vrsnak et al. 1991; Romano et al. 2003; Rust & LaBonte 2005; Williams et al. 2005; Chen et al. 2006).”
MAGNETIC FIELD STRUCTURES TRIGGERING SOLAR FLARES AND CORONAL MASS EJECTIONS (2012, background): “…et al. 2007; Wallace et al. 2010; Moore et al. 2011; Archontis & Hood 2012), multipolar 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…”
Numerical simulations of fast and slow coronal mass ejections (2007, result): “Some modellers reproduced the trajectories of individual filament eruptions and CMEs in good agreement with the observations (e.g., Krall et al. 2001; Chen & Krall 2003; Török & Kliem 2004, 2005; Williams et al. 2005; Chen et al. 2006).”
Solar filament eruptions and their physical role in triggering Coronal Mass Ejections (2012, background): “, 2012), twisted filaments/prominences (Williams et al., 2005; Koleva et al., 2012).”
The EUV Imaging Spectrometer for Hinode (2007, background): “In the case of eruption of twisted flux ropes (Williams et al., 2005), this removal process permits an eruption that is driven by the energy stored in the twisted field.”