By L. Mestel (auth.), O. Havnes, B. R. Pettersen, J. H. M. M. Schmitt, J. E. Solheim (eds.)

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Astrophys. Fluid Dyn. 34, 265. A. 1987a, J. Physics A, to appear. A. 1987b, preprint. A. B. Field 1984, J. Fluid Mech. 147, 133. A. H. Roberts 1987, Adv. Appl. , to appear. H. 1986, J. Plasma Phys. 35, 133. Chandrasekhar, s. 1961, 'Hydrodynamic and Hydromagnetic Stability', (Oxford: Oxford University Press). H. M. Antonsen 1985, Comments Plasma Phys. Contr. Fusion 9, 11. Heyvaerts, J. R. Priest 1984, Astron. Astrophys. 137, 63. H. S. Chu 1984, Phys. Fluids 27, 281. K. 1969, J. Fluid Mech. 35, 117.

H. : 1986, Adv. Space Res . 8, 235. L.

This coverage factor is too small to be measured by applying the same technique to the Sun as a star. g. Sun et al. 1987), it cannot be tested directly on disk integrated observations of the Sun. It is also important to remind that measurements using visible light refer to magnetic fields outside spot areas: since spots are much darker than the surrounding photosphere in visible light, their contribution to the integrated line profiles is expected to be negligible in typical stellar conditions.

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