Refraction in a pulsar magnetosphere - the effect of a variable emission height on pulse morphology

The Petrova (2000) model to calculate pulse profiles is extended to a variable emission height model to make it physically self-consistent. In this context variable means that the emission height is no longer considered to be the same for dierent magnetic field lines. The pulse profiles calculated using this new model seem to be less realistic due to a focusing e ect and cannot be used to fit (typical) multifrequency pulsar observations. Apart from the focusing eect the general morphology of pulse profiles is not greatly aected by introducing a variable emission height. Additional extensions of the model will be needed to be able to fit observations, and several suggestions are made.