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Chromospheres, Coronae and Mass Loss in Solar and Late-Type Stars
Published online by Cambridge University Press: 30 March 2016
Extract
Until observations in the EUV spectral region became available the existence of hot extended envelopes aroung latetype stars was inferred from the presence of visible and near infrared region lines which cannot be formed in radiative equilibrium within the stellar photospheres. The traditional indicators of stellar chromospheres have been the Ca II H and K lines, particularly the presence of emission components, the He I 10830 A triplet, the He II 4686 A line and emission in various hydrogen Balmer and Paschen lines. When observations from rockets and satellites become possible the strong lines of Mg II at 2800 A and the H Lya line at 1216 A could also be included in the modelling of stellar chromospheres. The new spectra from IUE allow not only stellar chromospheres to be studied but also stellar transition regions, should hot coronae exist.
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