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

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108, 322. : 1980, Astron. Nachr. 301, 18I. : 1986, Astron. Astrophys. 166,306. : 1987, in The Internal Solar Angular Velocity, eds. R. Durney and S. Sofia, D. Reidel, Dordrecht, p. 361. : 1987, Astron. Astrophys. 174,281. : 1985, Solar Phys. 95, 22I. : 1969, Astron. Nachr. 291,49. : 1986, Nature 319,285. : 1974, Astron. Astrophys. 37, 121. : 1983, Mitt. Astron. Ges. 60, 95. : 1984, Astron. Nachr. 305,225. : 1987, in The Internal Solar Angular Velocity, eds. R. Durney and S. Sofia, D. 83. : 1983, Monthly Notices Roy.

These and other problems shed a feeling of mistrust on magnetic field measurements, at least on the most simplified types of analysis used in interpreting the observations (Kurucz and Hartmann 1984; see also Hartmann 1987). Recently, Saar (1986, 1987; see also Linsky 19135) has made an attempt to overcome some of the main limitations of previous simplified analyses and has obtained a large number of magnetic field measurements in stars, which appear both more accurate and reliable. The improvements made by Saar are basically of two types: a) inclusion of radiative transfer effects; b) compensation for blends.

1981). This is also true for low resolution observations obtained with the Imaging Proportional Counter on EINSTEIN (Majer et al. 1986). Taken at face value, these two-temperature models suggest the existence on stars of separate regions in two quite distinct temperature regimes. Most likely, these two regions are formed by two families of loops with different physical conditions. Alternatively, the twotemperature solutions may be a consequence of poor spectral resolution and energy dependence of detector response when the source is characterized by a continuous emission measure distribution with temperature.

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