Pulsar Wind Nebulae as High Energy γ−Ray Emitters

There is growing evidence that some variable high-energy γ−ray sources are associated with pulsar wind nebulae. We review the current status of X-ray and radio studies of the sources most likely to be significant emitters above 100 MeV. The assumption of the γ−radiation arising from synchrotron processes puts a lower limit on the magnetic field and suggests there may be significant doppler boosting causing the asymmetries seen in the morphology of these nebulae. However, these sources are also in close proximity to molecular clouds, suggesting that variable γ−ray emission may arise from a ram pressure confined pulsar wind nebula in a dense medium.