Emergence of magnetic flux from the convection zone into the corona

By V. Archontis, F. Moreno-Insertis, K. Galsgaard, A. Hood, E. O'Shea. 2004

223 citations recorded by the source corpus.

Subfields: Astronomy and Astrophysics, Molecular Biology

View Paper: https://www.semanticscholar.org/paper/204c19ce963379c2ce0a2402de97b936459e7f20

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Citations in the corpus

The standard flare model in three dimensions II: upper limit on solar flare energy (2012, background): “…in past symmetric models (van Ballegooijen & Martens 1989; Amari et al. 2003), and they matched observations and simulations for active regions during their late flux emergence stage and their subsequent decay phase (e.g. van Driel-Gesztelyi et al. 2003; Archontis et al. 2004; Green et al. 2011).”
Solar Surface Emerging Flux Regions: A Comparative Study of Radiative MHD Modeling and Hinode SOT Observations (2008, background): “This behavior, which was originally predicted by Spruit, Title, & van Ballegooijen (1987), can also be found in previous idealized simulations of flux tubes emerging from the convection zone to the solar atmosphere (e.g. Magara 2001; Archontis et al. 2004).”
Jets in Coronal Holes: Hinode Observations and Three-dimensional Computer Modeling (2007, methodology): “The system is solved using the staggered-grid MHD code of our previous experiments (Nordlund & Galsgaard 1997; see Archontis et al. 2004).”
Coronal prominence structure and dynamics: A magnetic flux rope interpretation (2006, background): “instance, multiple reconnections are occurring along a single field line: this has been previously found to occur in the simulation of Archontis et al. [2005]. Figure 6d”
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).”
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 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).”
Eruption of magnetic flux ropes during flux emergence (2008, unknown): “The further rise into the atmosphere occurs by the development of a magnetic buoyancy instability (Archontis et al. 2004).”
SIMULATION OF THE FORMATION OF A SOLAR ACTIVE REGION (2010, methodology): “Complementing this line of work, multidimensional MHD simulations (e.g. Forbes & Priest 1984; Isobe et al. 2005; Shibata et al. 1989; Archontis et al. 2004; Manchester IV et al. 2004; Magara 2006; Fang et al. 2010) into the solar atmosphere have greatly improved our understanding of how the buoyant…”
THREE-DIMENSIONAL MODELING OF QUASI-HOMOLOGOUS SOLAR JETS (2010, background): “…confirmed that magnetic reconnection at a null point can explain numerous observable properties of jets (Yokoyama & Shibata 1995, 1996; Miyagoshi & Yokoyama 2004; Archontis et al. 2004, 2005, 2007; Galsgaard et al. 2007; Moreno-Insertis et al. 2008; Gontikakis et al. 2009; Archontis et al. 2010).”
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).”