the crust-core interface as well. However, for simplicity, in the present calculation we treat $g(r)$ as constant. We choose the following functional form for $f$: f()=[f\_0[(/\_0)\^2]{}]{}, \[fform\] where $\theta_0$ is an adjustable parameter defining how sharply the toroidal field rises away from the magnetic poles. The normalization constant $f_0$ is specified so that $\max[f(\theta)]=1$. Obviously, this functional form for $f(\theta)$ is representative; other forms are possible. However, the detailed shape of $f(\theta)$ cannot be realistically constrained and is not important for our purpose. Our goal is to examine what ranges of values of $B_0$ and $\theta_0$ are required in order to produce sufficiently distinct surface hot spots to generate the observed large pulse fraction in Kes 79 NS. Note that we are essentially exploring a parameter space orthogonal to the one considered by Geppert et al. (2006), who fixed $f(\theta)$ to be a simple sinusoid and explored the dependence of surface temperature and pulse shape on $g(r)$.

In addition to the crustal toroidal magnetic field, we also include a star-centered dipole field. The canonical surface dipole field strength (at the magnetic poles) as inferred from the $P$-$\dot P$ measurement is $B_p\sin\theta_B\simeq 6.2\times 10^{10}$ G (for $R=10$ km and moment of 