  Over the last fifty years since the discovery of pulsars, our understanding
of where and how pulsars emit the radiation we observe has undergone
significant revision. The location and mechanisms of high-energy radiation are
intimately tied to the sites of particle acceleration. The evolution of
emission models has paralleled the development of increasingly more sensitive
telescopes, especially at high energies. I will review the history of pulsar
emission modeling, from the early days of gaps at the polar caps, to outer gaps
and slot gaps in the outer magnetosphere, to the present era of global
magnetosphere simulations that locate most acceleration and high- energy
emission in the current sheets.
