are nevertheless representative of the pulse profiles that would be observed in energy bins centered on the quoted energies, with widths of a few tenths of a keV.

Although our theoretical light curves reproduce the large pulse fraction observed in the Kes 79 NS, there remains appreciable difference between the shape of the light curves presented in Figure 4 and the observation. Our model light curves have relatively sharp peaks, with the system spending nearly half of the rotation period at the (observed) flux minimum. This is different from the broad flux maximum observed in Kes 79 NS. Note, of course, that we have only considered one particular functional form for the magnetic field distribution, and the form we consider is very smooth. It is not clear that more complex magnetic field configurations would yield the right pulse shape while maintaining a high pulse fraction. Another possible way to resolve this difference is to consider pulse profiles with two peaks per rotation period, one peak for each magnetic hot spot. This is possible when both the line of sight and the magnetic dipole axis are nearly perpendicular to the rotation axis. Such a light curve would be observationally indistinguishable from 