The Thermal Evolution of Ultramagnetized Neutron Stars

Using recently calculated analytic and numerical models for the thermal structure of ultramagnetized neutron stars, we estimate the effects that ultrastrong magnetic fields $B \ge 10^{14}$ G have on the thermal evolution of a neutron star. Understanding this evolution is necessary to interpret models that invoke ``magnetars'' to account for soft $\gamma$-ray emission from some repeating sources.