A Flux-Tube Tectonics Model for Solar Coronal Heating Driven by the Magnetic Carpet
By Eric Priest, J. Heyvaerts, A. Title. 2002
211 citations recorded by the source corpus.
Subfields: Astronomy and Astrophysics
View Paper: https://www.semanticscholar.org/paper/fac3588c8ddafe8686aa5a90ed78a08b68a2b6a8
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In Astronomy and Astrophysics
- G. Aulanier
- P. Démoulin
- Etienne Pariat
- S. Cranmer
- A. A. Ballegooijen
- C. R. DeVore
- E. DeLuca
- Mahboubeh Asgari-Targhi
Citations in the corpus
- On Solving the Coronal Heating Problem (2005, background): “…fields containing separatrix surfaces, nulls, and separators (e.g., Karpen, Antiochos, and DeVore, 1996; Longcope, 1996, 1998; Aly and Amari, 1997; Priest, Heyvaerts, and Title, 2002); (2) complex photospheric flow patterns with stagnation points at the base of simple coronal magnetic fields…”
- Slip-Running Reconnection in Quasi-Separatrix Layers (2006, background): “The same physics is also invoked to model coronal heating when the photospheric distribution of flux shows multiple concentrations (e.g. Démoulin and Priest, 1997; Wang et al., 2000; Fletcher et al., 2001; Priest, Heyvaerts, and Title, 2002; Priest, Longcope, and Heyvaerts, 2005).”
- Solar Wind Electrons Alphas and Protons (SWEAP) Investigation: Design of the Solar Wind and Coronal Plasma Instrument Suite for Solar Probe Plus (2015, unknown): “…Dmitruk et al. (2002), Cranmer et al. (2007), Chandran et al. (2009) cBruner (1978), Ulmschneider (1985) dParker (1979, 1987), Sturrock (1999), Priest et al. (2002), Axford and McKenzie (1992), Cargill and Klimchuk (2004), Schrijver et al. (1997), Zurbuchen et al. (2002) eScudder (1994),…”
- HEATING OF THE SOLAR CHROMOSPHERE AND CORONA BY ALFVÉN WAVE TURBULENCE (2011, background): “The mis-alignment angle is much smaller than that required in quasi-static braiding models that match the observed heating rate (Parker 1983; Priest et al. 2002).”
- Flux tube texture of the solar wind: Strands of the magnetic carpet at 1 AU?: FLUX TUBE TEXTURE OF SOLAR WIND (2008, methodology): “…gaps in the magnetic carpet [cf. Close et al., 2004b]: these open-flux bundles will form flux tubes with a multitude of magnetic separatrices in the corona [e.g., Priest et al., 2002] (the separatrices being the flux tube walls), with about 5 separatrices per supergranule [Close et al., 2005].”