By L. Mestel (auth.), O. Havnes, B. R. Pettersen, J. H. M. M. Schmitt, J. E. Solheim (eds.)
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Extra info for Activity in Cool Star Envelopes
2: Left: The quantity on the left-hand side of eq. 16). Right: The same but for models with smoother and distributed profiles. "SK distributed" is a model with the error function profiles as used by Steenbeck and Krause, but smoother and overlapping. Models 1 and 2 refer to our model with a differential rotation profile from Hill (1987), taking a and 11 from the mixing length theory. 3. As a last point we plot in Fig. 8) as before. 7 and the scatter quite small. 8) are not necessarily linear in Q.
1975, Astrophys. f. Suppl. 29,467. : 1976, Solar Phys. 50, 3. THE DEVELOPMENT OF STRUCTURE IN CORONAL MAGNETIC FIELDS Mitchell A. Berger Department of Mathematical Sciences University of St Andrews Fife KY16 9SS Scotland ABSTRACT. Much of solar and stellar activity arises from the release of stored magnetic energy. This energy can often be associated with the existence of fieldline structures such as shear, twist, and braiding. At what rate does magnetic structure enter a coronal field? This paper discusses the growth of structure due to random photospheric motions.
Chu 1984, Phys. Fluids 27, 281. K. 1969, J. Fluid Mech. 35, 117. N. 1983, Ap. J. 298, 421. R. 1982, 'Solar Magnetohydrodynamics' , Reidel. H. D. Ursell 1960, Phil. Trans. Roy. Soc. London A252, 317 .. Rudnick, J. and Y. Hu , J. Physics A. 20, 4419. A. and Y. Uchida 1981, Ap. J. 246, 331. B. 1986, Rev. Mod. Phys. 58, 741. STELLAR MAGNETIC FIELDS: MEASUREMENTS AND DIAGNOSTICS R. Pallavicini Osservatorio Astrofisico di Arcetri Largo E. Fermi 5 50125 Firenze, Italy ABSTRACT. Magnetic fields are central to our understanding of surface activity in cool stars.
Activity in Cool Star Envelopes by L. Mestel (auth.), O. Havnes, B. R. Pettersen, J. H. M. M. Schmitt, J. E. Solheim (eds.)