Because of the corotation, the polarization angle (PA) curve of a pulsar lags
the intensity profile by 4r/Rlc rad in pulse phase. I present a simple and
short derivation of this delay-radius relation to show that it is not caused by
the aberration (understood as the normal beaming effect) but purely by
contribution of corotation to the electron acceleration in the observer's
frame. Available altitude-dependent formulae for the PA curve are expressed
through observables and emission altitude to make them immediately ready to use
in radio data modelling. The analytical approximations for the
altitude-dependent PA curve are compared with exact numerical results to show
how they perform at large emission altitudes. I also discuss several possible
explanations for the opposite-than-normal shift of PA curve, exhibited by the
pedestal emission of B1929+10 and B0950+08.Comment: 12 pages, 5 figures, accepted by MNRAS after minor change