a single-peaked light curve, but would imply that the actual rotation period of the NS is two times shorter.

Figure 5 presents several examples of the two-peaked light curves for different combinations of the geometric parameters $\beta$ and $\theta_B$ (both around $90^\circ$). We see that the width of the peaks is much closer to what is observed in Kes 79 NS. Obviously, when either $\beta$ or $\theta_B$ deviates significantly from $90^\circ$, the two peaks will have unequal heights, which can be measurable. Still, our result in Figure 5 shows that the square of geometrical phase space with corners at $(\beta,\theta_B)=(80^\circ,80^\circ)$ and (by symmetry) $(110^\circ,110^\circ)$ provides viable two-peaked light curves that may be indistinguishable from single-peaked light curves.

Discussion
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Large Pulse Fraction - How?
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Beloborodov (2002) demonstrated that two infinitesimal antipodal hot spots, emitting isotropically, on the surface of a $1.4\mathrm{M}_\mathrm{sun}$, $10$ km NS cannot, in full geometric generality, produce light curves with pulse fractions higher than about $12\%$. Poutanen & Beloborodov (2006) later generalized this to anisotropic emergent intensities, producing pulse fractions of $\mathrm{a~few}\times 10\%$. Thus, it seems that even if one were to find a way to create hot spots on the NS surface, it would be 