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The frequency dependence of pulse width is studied for 150 normal pulsars,mostly selected from the European Pulsar Network, for which the 10\%multifrequency pulse widths can be well fit with the Thorsett relationshipW_{10}=A\nu^{\mu}+W_{\rm 10, min}. The relative fraction of pulse width changebetween 0.4~GHz and 4.85~GHz, \eta=(W_{4.85}-W_{0.4})/W_{0.4}, is calculated interms of the best-fit relationship for each pulsar. It is found that 81 pulsars(54\%) have $\eta<-10$\% (group A), showing considerable profile narrowing athigh frequencies, 40 pulsars (27\%) have $-$10\%$\leq\eta\leq 10$\% (group B),meaning a marginal change in pulse width, and 29 pulsars (19\%) have$\eta>10$\% (group C), showing a remarkable profile broadening at highfrequencies. The fractions of the group-A and group-C pulsars suggest that theprofile narrowing phenomenon at high frequencies is more common than theprofile broadening phenomenon, but a large fraction of the group-B and group-Cpulsars (a total of 46\%) is also revealed. The group-C pulsars, together witha portion of group-B pulsars with a slight pulse broadening, can hardly beexplained using the conventional radius-to-frequency mapping, which onlyapplies to the profile narrowing phenomenon. Based on a recent version of thefan beam model, a type of broadband emission model, we propose that the diversefrequency dependence of pulse width is a consequence of different types ofdistribution of emission spectra across the emission region. The geometricaleffect predicting a link between the emission beam shrinkage and the spectrumsteepening is tested but disfavored.

Frequency dependence of pulse width for 150 radio normal pulsars