Astrophys. J., Suppl. Ser., 215, 11 (2014/November-0)
Frequency dependence of pulse width for 150 radio normal pulsars.
CHEN J.L. and WANG H.G.
Abstract (from CDS):
The frequency dependence of the 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 relationship W10= Aνµ + W_10, min_. The relative fraction of pulse width change between 0.4 GHz and 4.85 GHz, η = (W4.85- W0.4)/W0.4, is calculated in terms of the best-fit relationship for each pulsar. It is found that 81 pulsars (54%) have η < -10% (group A), showing considerable profile narrowing at high frequencies, 40 pulsars (27%) have -10% ≤ η ≤ 10% (group B), meaning a marginal change in pulse width, and 29 pulsars (19%) have η > 10% (group C), showing a remarkable profile broadening at high frequencies. The fractions of the group-A and group-C pulsars suggest that the profile narrowing phenomenon at high frequencies is more common than the profile broadening phenomenon, but a large fraction of the group-B and group-C pulsars (a total of 46%) is also revealed. The group-C pulsars, together with a portion of group-B pulsars with slight pulse broadening, can hardly be explained using the conventional radius-to-frequency mapping, which only applies to the profile narrowing phenomenon. Based on a recent version of the fan beam model, a type of broadband emission model, we propose that the diverse frequency dependence of pulse width is a consequence of different types of distribution of emission spectra across the emission region. The geometrical effect predicting a link between the emission beam shrinkage and spectrum steepening is tested but disfavored.
methods: statistical - pulsars: general - radiation mechanisms: non-thermal
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