By A.L. Septier

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Scharmer, K. Bjelksjo, T. Korhonen, B. Lindberg, B. Petterson, in Proceedings of SPIE in Innovative Telescopes and Instrumentation for Solar Astrophysics, vol. 4853 ed. L. V. Avakyan, p. B. R. Sheeley Jr, Astrophys. J. R. Sheeley Jr, Sol. Phys. 1, 171 (1967) L. Spitzer in Proceedings of 2-nd International Conference Atoms for Peace. (Geneva 1958), p. C. Spruit, Astron. Astrophys. 98, 155 (1981) O. Steiner, U. Grossmann-Doerth, M. Knoelker, M. Schuessler, Astrophys. J. 495, 468 (1998) O. Steiner, AIP Conf.

Their length may be more than solar radius. , the quiescent prominences overhang the corona. At the same time the mass density of prominences is by 2–3 orders of magnitude higher than the coronal plasma density. In other words, a heavy cool material of prominence suspended over rarefied hot gas is like an iron bar floating in thin air. 11 shows the sun in 304 Å He II line (5 × 104 K) taken by the SDO/AIA instrument on November 13, 2011 together with the HMI magnetogram. The red lines on the magnetogram follow the path of prominences suspended above the demar- 16 1 The Sun’s Magnetic Fields cation line dividing the quiet sun magnetic network of opposite polarities.

The magnetic field in these small magnetic features was found to range from 200 to 700 G. ” His conclusion, that “magnetic fields of several hundred gauss occur in tiny areas easily as small as 500 km in regions of the solar surface sometimes well removed from sunspot activity,” became the turning point which, despite the predecessors, is a fact of the discovery of small scale flux tubes. 5−2 ) is about 1,400 G. ), much higher than the average field of the sunspot itself. He also observed an isolated places outside sunspots having field strengths up to 1,000 G.

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