Published online by Cambridge University Press: 23 September 2016
The magnetic-loop model for a stellar mantle is described and it is shown how this model may be used to understand the differences in spectrum and change of spectrum which are observed for main-sequence stars haying effective.temperatures in the range from 2.5 x 104 to 3.0 x 104 K.
It is suggested that the difference in spectrum between a shell star such as Gamma Cas when it is in an active state and a Wolf-Rayet star may be due to a difference in environment.