The effect of magnetospheric refraction on the morphology of pulsar profiles

Refraction of ordinary superluminous waves in an ultrarelativistic highly m agnetized plasma of pulsars is considered. The effect is found to cause an essential redistribution of rays in final directions which leads to the for mation of separate components in pulse profiles. It is shown that refractio n of waves in pulsar magnetospheres can account for the main features of pr ofile morphology given that the hollow-cone emission model is the case. The observed frequency evolution of pulsar profiles appears to be well explain ed by the frequency dependence of the refraction efficiency if one also tak es into account the effects of observational geometry. Special attention is paid to the interpretation of the inner conal components within the frame of our model.