Editing Stellar corona (section)

====Large-scale structures====
Large-scale structures are very long arcs which can cover over a quarter of the solar disk but contain plasma less dense than in the coronal loops of the active regions.

They were first detected in the June 8, 1968, flare observation during a rocket flight.<ref name = Giacconi>{{cite conference |last = Giacconi| first = Riccardo| title = G. S. Vaiana memorial lecture |book-title=Physics of Solar and Stellar Coronae: G.S. Vaiana Memorial Symposium: G.S. Vaiana Memorial Symposium : Proceedings of a Conference of the International Astronomical Union |editor-first1=J. F. |editor-last1=Linsky |editor-first2=S. |editor-last2=Serio| pages = 3–19 | year = 1992 | publisher = Kluwer Academic |location=Netherlands | isbn = 978-0-7923-2346-4}}</ref>

The large-scale structure of the corona changes over the 11-year solar cycle and becomes particularly simple during the minimum period, when the magnetic field of the Sun is almost similar to a dipolar configuration (plus a quadrupolar component).