Turkish Journal of Physics




The wealth of astronomical observations obtained in the extreme ultraviolet in recent years, have allowed comprehensive studies of the stellar transition regions and coronae to be carried out. For the first time we have been able to resolve individual coronal lines of various elements formed over a large temperature range (10^{5} - 10^{7.2} K). The temperature, densities, abundances and magnetic field strengths of the stellar coronae can now be determined. Here we review some of the observations in the field of cool stars and discuss the implications on atmospheric heating requirements.

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