There is a clear need for the further applications of this method to CP1, CP3 and CP4 stars, to have a large amount of data from which it would be possible to analyse the problems of effective temperature, classification and atmosphere modeling of CP stars. There is also a need to study the effective temperature and the Balmer jump variations with a phase for stars with enough number of the individual scans.
The author would like to thank Drs. V.A. Hagen-Thorn, I.M. Kopylov and I.S. Guseva for their helpful comments. This work has been supported by the Russian National Foundation for Astronomy (project No. 220.127.116.11).
Copyright The European Southern Observatory (ESO)