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In this paper we explore the evolution of a PWN while the pulsar is spinningdown. An MHD approach is used to simulate the evolution of a composite remnant.Particular attention is given to the adiabatic loss rate and evolution of thenebular field strength with time. By normalising a two component particleinjection spectrum (which can reproduce the radio and X-ray components) at thepulsar wind termination shock to the time dependent spindown power, and keepingtrack with losses since pulsar/PWN/SNR birth, we show that the average fieldstrength decreases with time as $t^{-1.3}$, so that the synchrotron fluxdecreases, whereas the IC gamma-ray flux increases, until most of the spindownpower has been dumped into the PWN. Eventually adiabatic and IC losses willalso terminate the TeV visibility and then eventually the GeV visibility.

Unidentified Gamma-Ray Sources as Ancient Pulsar Wind Nebulae