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We present the results of detailed spatial and spectral analysis of thepulsar wind nebula (PWN) in supernova remnant Kes 75 (G29.7-0.3) using a deepexposure with Chandra X-ray observatory. The PWN shows a complex morphologywith clear axisymmetric structure. We identified a one-sided jet and two brightclumps aligned with the overall nebular elongation, and an arc-like featureperpendicular to the jet direction. Further spatial modeling with a torus andjet model indicates a position angle $207\arcdeg\pm8 \arcdeg$ for the PWNsymmetry axis. We interpret the arc as an equatorial torus or wisp and theclumps could be shock interaction between the jets and the surrounding medium.The lack of any observable counter jet implies a flow velocity larger than0.4c. Comparing to an archival observation 6 years earlier, some small-scalefeatures in the PWN demonstrate strong variability: the flux of the inner jetdoubles and the peak of the northern clump broadens and shifts 2" outward. Inaddition, the pulsar flux increases by 6 times, showing substantial spectralsoftening from $\Gamma$=1.1 to 1.9 and an emerging thermal component which wasnot observed in the first epoch. The changes in the pulsar spectrum are likelyrelated to the magnetar-like bursts of the pulsar that occurred 7 days beforethe Chandra observation, as recently reported from RXTE observations.

Deep Chandra Observation of the Pulsar Wind Nebula Powered by the Pulsar J1846-0258 in the Supernova Remnant Kes 75