Eruption of a Buoyantly Emerging Magnetic Flux Rope

By W. Manchester IV, Tamas I. Gombosi, D. Dezeeuw, Yuhong Fan. 2003

283 citations recorded by the source corpus.

View Paper: https://www.semanticscholar.org/paper/1925a688c685b75f78bc8f4f24042bb143981dd2

How researchers see this paper

The researchers whose trusted networks rank it highest, strongest advocate first. Every researcher gets a different order.

In Astronomy and Astrophysics

Citations in the corpus

Solar Surface Emerging Flux Regions: A Comparative Study of Radiative MHD Modeling and Hinode SOT Observations (2008, background): “In light of the work by Manchester et al. (2004) and Magara (2006), who reported that the expansion of rising twisted magnetic tubes into the solar atmosphere drives systematic shear flows, it is expected that the shearing term becomes increasingly important towards the surface.”
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).”
Solar filament eruptions and their physical role in triggering Coronal Mass Ejections (2012, background): “The flux rope flattens below the photosphere and only fragmented sections can progressively reach the top of the photosphere (Manchester et al., 2004; Magara, 2006; Archontis et al., 2009).”
Coronal prominence structure and dynamics: A magnetic flux rope interpretation (2006, methodology): “Although there were no rotational motions induced by the kink instability as in our simulation, significant shearing motions induced by axial field gradients occurred oppositely directed across the neutral line, and were critical to the rope’s bifurcation [ Manchester et al., 2004 ].”
Physics of Solar Prominences: II—Magnetic Structure and Dynamics (2010, background): “…have shown that during the process of flux emergence, after the top of the flux rope has emerged, magnetic reconnection or helicity injection (Manchester et al., 2004; Magara, 2006; Archontis and Török, 2008; Fan, 2009) may reconfigure the emerged coronal arcade to produce a secondary…”
The Three-dimensional Interaction between Emerging Magnetic Flux and a Large-Scale Coronal Field: Reconnection, Current Sheets, and Jets (2005, background): “…of years now (Matsumoto & Shibata 1992; Matsumoto et al. 1993, 1998; Kusano et al. 1998; Fan 2001; Magara & Longcope 2001; 2003; Abbett & Fisher 2003; Archontis et al. 2004; Manchester et al. 2004; see the introduction of the paper by Archontis et al. 2004 for a detailed history of the subject).”
THE EMERGENCE OF A TWISTED FLUX TUBE INTO THE SOLAR ATMOSPHERE: SUNSPOT ROTATIONS AND THE FORMATION OF A CORONAL FLUX ROPE (2009, background): “…flux rope with sigmoid-shaped concave upturning field lines threading under a central axis that rises into coronal heights is found to develop in the end in many simulations (e.g. Magara and Longcope 2001, 2003; Magara 2004; Manchester et al. 2004; Magara 2006; Archontis and Toëroëk 2008).”
Eruption of magnetic flux ropes during flux emergence (2008, unknown): “In this framework, Manchester et al. (2004) simulated the emergence of a twisted flux tube into a non-magnetized, stratified atmosphere and reported the formation of a distinct magnetic flux rope within the emerging tube, when the length of the buoyant part of the tube is small.”
Onset of Coronal Mass Ejections Due to Loss of Confinement of Coronal Flux Ropes (2007, background): “…flux rope, it was shown (Gibson & Fan 2006a, 2006b) that the writhing of the rope and the collapsing together of its two legs results in internal reconnections that separate the rope, leaving behind the lower dipped field of the flux rope (see also Gilbert et al. 2001; Manchester et al. 2004).”
Adaptive numerical algorithms in space weather modeling (2012, methodology): “Currently the physics-based EE model only works in a stand-alone mode [30,31], and we use the empirical models to generate CMEs in the SWMF [32,33].”
DIRECT EVIDENCE FOR A FAST CORONAL MASS EJECTION DRIVEN BY THE PRIOR FORMATION AND SUBSEQUENT DESTABILIZATION OF A MAGNETIC FLUX ROPE (2012, background): “…et al. 1999; Amari et al. 2000; Lynch et al. 2008; Vršnak 2008), or in the photosphere or low chromosphere, photospheric flux rope (e.g., Magara & Longcope 2001; Manchester et al. 2004; Gibson & Fan 2006; Archontis & Hood 2008) after the emergence of a twisted flux tube from the convection zone.”
Three-dimensional MHD Simulation of the 2003 October 28 Coronal Mass Ejection: Comparison with LASCO Coronagraph Observations (2008, methodology): “…of Hawaii, Honolulu, Hawaii 4 George Mason University, Fairfax, Virginia 1 specific CME simulations (e.g. Usmanov & Dryer 1995; Riley et al. 2002; Manchester et al. 2004b; Jacobs et al. 2007), and non-event-specific Sun-to-thermosphere space weather simulations modeled by the Center for Space…”