Injection of Magnetic Energy and Magnetic Helicity into the Solar Atmosphere by an Emerging Magnetic Flux Tube

By T. Magara, D. Longcope. 2003

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In Astronomy and Astrophysics

Citations in the corpus

Numerical Simulations of Three-dimensional Coronal Magnetic Fields Resulting from the Emergence of Twisted Magnetic Flux Tubes (2004, background): “Hence, the outstanding question concerning how a twisted flux tube, carrying the dense plasma from the solar interior, can emerge as a whole through the photosphere boundary into the rarefied corona (Fan 2001; Magara & Longcope 2001, 2003) is not addressed.”
Emergence of magnetic flux from the convection zone into the corona (2004, unknown): “…the tradition in flux emergence calculations (e.g., Shibata et al. 1989; Nozawa et al. 1992; Matsumoto et al. 1993; Krall et al. 1998; Fan 2001; Magara & Longcope 2003), for the atmosphere we take two isothermal ranges (which, for brevity, we call the low atmosphere and the corona,…”
Magnetic Fields in the Solar Convection Zone (2004, background): “…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).”
Solar Surface Emerging Flux Regions: A Comparative Study of Radiative MHD Modeling and Hinode SOT Observations (2008, background): “In fact, Magara & Longcope (2003) finds from their emerging flux simulations that although the shearing term is initially smaller than the emergence term (for the photospheric base), the shearing term persists longer and becomes the dominant contributor to helicity injection into the solar…”
The magnetic field in the solar atmosphere (2014, background): “Magara and Longcope (2003) proposed that the helicity contribution from the vertical flows might only dominate early phases of flux emergence, followed by a dominant contribution from the shearing flows in the later stages of an evolving AR.”
The Three-dimensional Interaction between Emerging Magnetic Flux and a Large-Scale Coronal Field: Reconnection, Current Sheets, and Jets (2005, background): “…corona have also been available for a number 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…”
Eruption of a Buoyantly Emerging Magnetic Flux Rope (2003, background): “These photospheric temporal trends confirm what was found by Magara & Longcope (2003).”
THE EMERGENCE OF A TWISTED FLUX TUBE INTO THE SOLAR ATMOSPHERE: SUNSPOT ROTATIONS AND THE FORMATION OF A CORONAL FLUX ROPE (2009, background): “…(Shibata et al. 1989), a large body of 3D MHD simulations of the emergence of twisted magnetic flux tubes into the solar atmosphere (e.g. Fan 2001; Magara and Longcope 2001, 2003; Magara 2004; Manchester et al. 2004; Archontis et al. 2004; Murray et al. 2006; Magara 2006; Archontis and Toëroëk…”
The Emergence of a Twisted Magnetic Flux Tube into a Preexisting Coronal Arcade (2003, methodology): “In Magara & Longcope (2003), the axial field line of their left-hand–twisted emerging tube shows a slight inverse-S shape (see their Figs.”
Magnetic flux emergence in granular convection: radiative MHD simulations and observational signatures (2007, background): “The focus of most studies in the literature has been on the evolution of the emerging magnetic field in the corona (Fan, 2001; Magara, 2001; Magara & Longcope, 2003; Fan & Gibson, 2004; Abbett & Fisher, 2003; Archontis et al., 2004, 2005; Török & Kliem, 2005; Isobe et al., 2005; Galsgaard et al.,…”