The Thermal Evolution of Ultramagnetized Neutron Stars

Abstract

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 $γ$-ray emission from some repeating sources.