A Model for the Emergence of a Twisted Magnetic Flux Tube

By D. Longcope, B. Welsch. 2000

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Coronal prominence structure and dynamics: A magnetic flux rope interpretation (2006, methodology): “This and other simulations [Longcope and Welsch, 2000; Amari et al., 2004b; Archontis et al., 2005] indicate that even when a flux rope does not smoothly emerge across the photosphere, most or all of its axial flux can still be transported into the corona.”
Magnetic Fields in the Solar Convection Zone (2004, methodology): “Furthermore, based on a simplified model of active region flux emergence into the corona by Longcope and Welsch (2000), Fan et al. (2009) show that a stronger field strength in the leading tube also produces a faster rotation of the leading polarity sunspot driven by torsional Alfvén waves along…”
THE EMERGENCE OF A TWISTED FLUX TUBE INTO THE SOLAR ATMOSPHERE: SUNSPOT ROTATIONS AND THE FORMATION OF A CORONAL FLUX ROPE (2009, background): “…along the twisted flux tube, transporting magnetic twist from the tube’s interior portion, where the rate of twist is high, to its greatly stretched coronal portion, where the rate of twist is low, a result that was predicted by an earlier idealized analytical model of Longcope and Welsch (2000).”
Driving major solar flares and eruptions: A review (2008, result): “Work by Longcope and Welsch (2000) supports this finding.”