The Nonpotentiality of Active-Region Coronae and the Dynamics of the Photospheric Magnetic Field

By C. Schrijver, M. DeRosa, A. Title, T. Metcalf. 2005

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In Astronomy and Astrophysics

Citations in the corpus

EVOLUTION OF MAGNETIC FIELD AND ENERGY IN A MAJOR ERUPTIVE ACTIVE REGION BASED ON SDO/HMI OBSERVATION (2011, background): “2, 37191 Katlenburg-Lindau, Germany. rectly monitors the AR’s evolution and provides information on its non-potential nature (e.g. Schrijver et al. 2005).”
Nonlinear Force-free Field Modeling of a Solar Active Region around the Time of a Major Flare and Coronal Mass Ejection (2007, background): “…of preexisting magnetic flux by plasma flows on the surface (e.g., Leka et al. 1996; Wheatland 2000; Démoulin et al. 2002b, 2002a; Falconer et al. 2002; Leka & Barnes 2003a, 2003b; Schrijver et al. 2005; Wiegelmann et al. 2005; Régnier & Canfield 2006; Jing et al. 2006; Schrijver 2007).”
THE NATURE OF FLARE RIBBONS IN CORONAL NULL-POINT TOPOLOGY (2009, background): “Significant flux emergence occurring within an active region is usually a strong precursor of a flare activity (e.g., Schrijver et al. 2005; Schrijver 2009).”
COEXISTING FLUX ROPE AND DIPPED ARCADE SECTIONS ALONG ONE SOLAR FILAMENT (2010, methodology): “…is to use photospheric vector magnetograms as boundary conditions for the computation of NLFFFs in the corona, since, in active regions, in particular with complicated magnetic field structures, the force-free parameter α usually changes in space (Régnier et al. 2002; Schrijver et al. 2005).”
Nonlinear Force-Free Modeling of Coronal Magnetic Fields Part I: A Quantitative Comparison of Methods (2006, background): “Such models, although often fairly good approximations (e.g., Schrijver et al., 2005), cannot be used to determine the energy contained in electrical currents and magnetic fields available for driving instabilities, or even provide the simple assessment of where such energy might exist within…”
Photospheric Magnetic Field Properties of Flaring versus Flare-quiet Active Regions. IV. A Statistically Significant Sample (2007, result): “The first of these is consistent with the results of Schrijver et al. (2005), who found that the rate of flaring is significantly higher for rapidly evolving active regions.”
Solar Force-free Magnetic Fields (2012, methodology): “For example, a comparison of global potential fields with images from the Transition Region And Coronal Explorer (TRACE) done by Schrijver et al. (2005) and with stereoscopically-reconstructed loops by Sandman et al. (2009) showed large deviations between potential magnetic field lines and coronal…”
An Observational Overview of Solar Flares (2011, background): “They follow the rate of evolution of the active region (Schrijver et al. 2005) and require the presence of strong magnetic gradients(Hagyard et al. 1984).”
Tracking Vector Magnetograms with the Magnetic Induction Equation (2008, background): “…flux cancellation of the overlying coronal field (Linker et al. 2001), flux injection (Chen 1989, 1996), the kink instability of filaments (Rust & Kumar 1996; Török et al. 2004; Kliem et al. 2004), and photospheric footpoint shearing (Amari et al. 2000, 2003a, 2003b; Schrijver et al. 2005).”
Driving major solar flares and eruptions: A review (2008, background): “It appears that such currents survive for typically only a day, while powering one or more flares during their decay (e.g., Pevtsov et al. 1994; Burnette et al. 2004; Schrijver et al. 2005).”
HEATING OF THE SOLAR CHROMOSPHERE AND CORONA BY ALFVÉN WAVE TURBULENCE (2011, background): “Effects of Coronal Loop Expansion Models of the coronal magnetic field (e.g., Schrijver et al. 2005) predict that the field strengthB0 generally decreases with height in the corona.”