A study of the development in the solar corona of active centers born during the CSSAR period leads to the following remarks: the ‘enhancement’ of coronal emissions seems to take place first within a localized ‘core’ close to the plage, then to extend to a much larger ‘halo’; the core from which all the radiations under study originate does not last much more than the spots, whereas the ‘halo’ is characterized by the major importance of the emission at 5303 Å, and lasts as long as the K 3 plages. These features can be explained by the assumption that the enhancement is inhomogeneous during the first part of its life, then becomes homogeneous after the core has disappeared.