Empirical Constraints on Coronal Heating Processes
Observations of the transition regions and coronae of main-sequence stars that constrain coronal heating theories are reviewed. The significance of the form of the emission measure distribution and of correlations between transition region and coronal fluxes is discussed. Existing measurements of emission line widths place limits on the available wave flux. Correlations can be found between coronal parameters and stellar rotation rates, without knowledge of the heating mechanism. Measurements of surface magnetic fields and their dependence on rotation are vital in understanding coronal heating. At present, heating via stochastic or twisted fields seems the most plausible mechanism.
KeywordsEmission Measure Coronal Magnetic Field Coronal Heating Surface Magnetic Field Wave Flux
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