What is the source of the magnetic helicity shed by CMEs? The long-term helicity budget of AR 7978

By P. Démoulin, C. Mandrini, L. Driel-Gesztelyi, Barbara J. Thompson, S. Plunkett, Zsolt Kovári, G. Aulanier, A. Young. 2002

182 citations recorded by the source corpus.

Subfields: Astronomy and Astrophysics

View Paper: https://www.semanticscholar.org/paper/0d9f4ab85045a2c55dc3b3f0789609bd421df35f

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In Astronomy and Astrophysics

Citations in the corpus

Interplanetary flux rope ejected from an X-ray bright point. The smallest magnetic cloud source-region ever observed (2005, result): “Third, it is a simple and isolated magnetic bipole, well separated from other ARs (by at least half solar radius) but it was still eruptive.”
The solar magnetic field (2006, background): “ which ows along these eld lines. Especially in active regions these currents may be appreciable and lead to marked deviations of the shape of observed loops and their models based on a potential eld [509, 510, 511, 512, 513]. A substantial current was also found by [514] when they tried to match th”
The Magnetic Helicity Budget of Solar Active Regions and Coronal Mass Ejections (2003, methodology): “Démoulin et al. (2002b) assumed that each CME ejected from the active region they studied produced an MC.”
Solar filament eruptions and their physical role in triggering Coronal Mass Ejections (2012, background): “The long term diffusion of an AR was studied by Démoulin et al. (2002) and they reported that the rate of CMEs stayed nearly constant in the decaying AR during five months after the emergence phase.”
Coronal Mass Ejection: Initiation, Magnetic Helicity, and Flux Ropes. II. Turbulent Diffusion-driven Evolution (2003, background): “They are observed indeed to be produced in the phase of appearance and development of such regions, but also, although at a slower rate, during their longer dispersion phase (Démoulin et al. 2002).”
Eruption of magnetic flux ropes during flux emergence (2008, unknown): “On the other hand, the occurrence of CMEs in active regions, in their early phase of formation (e.g. Démoulin et al. 2002; Nindos et al. 2003), suggest that emerging flux carries the potential to produce eruptions by itself.”
Photospheric flux density of magnetic helicity (2005, background): “The flux of magnetic helicity from differential motion is usually found to be too small (typically a factor 10) to explain the helicity ejected in CMEs Appendix A is only available in electronic form at http://www.edpsciences.org (Démoulin et al. 2002; Green et al. 2002; Nindos et al. 2003).”
The Nonpotentiality of Active-Region Coronae and the Dynamics of the Photospheric Magnetic Field (2005, result): “Our study indirectly suggests that any such helicity buildup is likely related to flux emergence within a 20 hr period before the coronal observation, consistent with the conclusions reached by Wheatland (2000a) and by Démoulin et al. (2002a, 2002b) for the study of AR 7978.”