Transient Coronal Sigmoids and Rotating Erupting Flux Ropes

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Photospheric flux cancellation and associated flux rope formation and eruption (2010, background): “Since sigmoids form in the lower surface of their host flux ropes (Titov & Démoulin 1999; Green et al. 2007), a sigmoid in a BPSS flux rope forms in the bottom part of the BPSS and is likely to survive the eruption, at least partly.”
Solar filament eruptions and their physical role in triggering Coronal Mass Ejections (2012, background): “…in the photosphere (e.g., Liu et al., 2012a), or indirectly with the presence of J-shaped ribbons (e.g., Chandra et al., 2009), X-ray sigmoids (Green et al., 2007; McKenzie and Canfield, 2008; Liu et al., 2010; Savcheva et al., 2012), twisted filaments/prominences (Williams et al., 2005;…”
The Physical Processes of CME/ICME Evolution (2017, background): “When viewed from above, clockwise (anti-clockwise) rotation is typically observed for filaments erupting from source regions with positive (negative) helicity (Green et al. 2007; Fig.”
A MODEL FOR MAGNETICALLY COUPLED SYMPATHETIC ERUPTIONS (2011, background): “The rope rotates counterclockwise about its rise direction (as seen from above), due to the conversion of its twist into writhe (e.g., Green et al. 2007).”
EUV WAVE REFLECTION FROM A CORONAL HOLE (2009, background): “However, If the flux rope has an azimuthal component of the speed (see, e.g., Green et al., 2007), one can expect the wave driven by it to have an azimuthal component as well.”