SIMBAD references

An HR diagram annotated to show several ranges of photometerically determined periods has been constructed for the magnetic CP stars whose periods have been determined by the author and his collaborators. The distribution of periods reflects both the initial conditions as well as the subsequent stellar histories. Since the stellar magnetic field does not penetrate the convective core, eventually a shear zone near the core-radiative envelope boundary may develop which produces turbulence and modifies the field. Many, but not all, of the most rapidly rotating mCP stars are close to the ZAMS and some of the least rapidly rotating mCP stars are the furthest from the ZAMS.