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Unidentified Gamma-Ray Sources as Ancient Pulsar Wind Nebulae · Around

2009

Unidentified Gamma-Ray Sources as Ancient Pulsar Wind Nebulae

de Jager, O. C., Ferreira, S. E. S., Djannati-Ataï, A. et al.

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In this paper we explore the evolution of a PWN while the pulsar is spinning down.

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 the nebular field strength with time.
By normalising a two component particle injection spectrum (which can reproduce the radio and X-ray components) at the pulsar wind termination shock to the time dependent spindown power, and keeping track with losses since pulsar/PWN/SNR birth, we show that the average field strength decreases with time as $t^{-1.3}$, so that the synchrotron flux decreases, whereas the IC gamma-ray flux increases, until most of the spindown power has been dumped into the PWN.

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Then

Porter, T.A., Moskalenko, I.V. & Strong, A.W. 2006, ApJL, 648, L29
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