The Emergence of a Twisted Ω-Tube into the Solar Atmosphere

By Yuhong Fan. 2001

280 citations recorded by the source corpus.

View Paper: https://www.semanticscholar.org/paper/644d877221db2800198842dbadcb1cdd1279eccd

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In Astronomy and Astrophysics

Citations in the corpus

Physics of Solar Prominences: II—Magnetic Structure and Dynamics (2010, background): “…rise to coronal heights characteristic of quiet-Sun and intermediate prominences, even without the inhibiting presence of a preexisting coronal field (Fan, 2001; Archontis et al., 2004; Manchester et al., 2004; Magara, 2006; Galsgaard et al., 2007; Magara et al., 2008; Archontis and Török, 2008).”
The Origin, Early Evolution and Predictability of Solar Eruptions (2018, background): “Simulations that followed (Manchester, 2001; Fan, 2001; Magara and Longcope, 2003; Török et al, 2014) found that under these circumstances, shear flows develop spontaneously where horizontal flows reverse direction across emerging loop structures.”
The Three-dimensional Interaction between Emerging Magnetic Flux and a Large-Scale Coronal Field: Reconnection, Current Sheets, and Jets (2005, methodology): “The background stratification and magnetic tube parameters are the same as those used in Paper I and follow the general guidelines of the initial condition of Fan (2001).”
Eruption of a Buoyantly Emerging Magnetic Flux Rope (2003, methodology): “We show that the shorter section of rope bends more sharply and, having fewer turns, drains plasma more effectively than in the case of Fan (2001).”
Resistive Emergence of Undulatory Flux Tubes (2004, background): “…development of small-scale spatial undulations in subphotospheric flattened flux tubes (stable to the Parker instability; see Magara 2001) and the existence of magnetic dips at the bottom of emerging twisted flux tubes (in which dense material is trapped; see Magara & Longcope 2001 and Fan 2001).”
The Magnetic Connection between the Convection Zone and Corona in the Quiet Sun (2007, background): “There have been a number of attempts to simultaneouslymodel the ideal magnetohydrodynamic (MHD) evolution of the up- per convection zone and corona, mostly in the context of studies of emerging active regions (Fan 2001; Magara 2004, 2006; Manchester et al. 2004; Archontis et al. 2006).”
The Emergence of a Twisted Magnetic Flux Tube into a Preexisting Coronal Arcade (2003, background): “Hence, the outstanding question concerning the complex dynamics of how a twisted flux tube can emerge as a whole from the high-b interior through the photosphere boundary into the rarefied corona (Fan 2001; Magara & Longcope 2001, 2003) is not addressed.”
Coronal prominence structure and dynamics: A magnetic flux rope interpretation (2006, background): “One possibility is that ropes emerge from below the solar photosphere, having been already formed in the solar interior [Rust and Kumar, 1994; Low, 1996; Fan, 2001; Magara and Longcope, 2001; Abbett and Fisher, 2003; Archontis et al., 2004; Amari et al., 2004a, 2004b].”
Numerical Simulations of Three-dimensional Coronal Magnetic Fields Resulting from the Emergence of Twisted Magnetic Flux Tubes (2004, background): “Simulations of the emergence of twisted flux tubes into the solar atmosphere (Fan 2001; Magara & Longcope 2001) have shown that one can readily find emerged field lines displaying both forward-S and inverse-S morphologies for an emerging flux tube with one sign of twist.”
THE EMERGENCE OF A TWISTED FLUX TUBE INTO THE SOLAR ATMOSPHERE: SUNSPOT ROTATIONS AND THE FORMATION OF A CORONAL FLUX ROPE (2009, background): “With time the two polarity regions on the photosphere begin to show a significant shearing motion along the neutral line (e.g. Manchester 2001; Manchester et al. 2004; Fan 2001; Magara and Longcope 2003; Magara 2004, 2006), and the two polarity regions begin to separate.”
Magnetic Fields in the Solar Convection Zone (2004, methodology): “…on the photosphere initially emerge as north-south oriented, and then they undergo shearing motion along the polarity inversion line and separate in the east-west direction (e.g. Fan, 2001b; Magara and Longcope, 2003; Manchester IV et al., 2004; Archontis et al., 2004; Magara, 2006; Fan, 2009b).”
Emergence of magnetic flux from the convection zone into the corona (2004, unknown): “As in previous flux emergence calculations (e.g., Fan 2001; Magara & Longcope 2001), we choose helical field lines highly twisted around the central axis (albeit with constant pitch): Bϕ = αrBy.”
Photospheric flux cancellation and associated flux rope formation and eruption (2010, background): “Numerical simulations of the bodily emergence of a flux rope indicate that the process essentially stops as the magnetic axis of the rope reaches the photosphere, producing a sheared arcade in the corona (Fan 2001).”
Onset of Coronal Mass Ejections Due to Loss of Confinement of Coronal Flux Ropes (2007, background): “…that it is difficult for a twisted flux tube to rise bodily into the corona as a whole due to the heavy plasma that is trapped at the bottom concave (U-shaped) portions of the winding field lines, and the axis of the flux tube barely rises above the photosphere (Fan 2001; Archontis et al. 2004).”