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We report on the results of Chandra X-ray observations of the $\gamma$-rayradio-quiet pulsar J1932+1916. We confirm the previous detection of the pulsarcounterpart and its pulsar wind nebula in X-rays from low spatial resolutiondata obtained by Suzaku and Swift. The Chandra data with much better spatialresolution resolved the fine structure of the nebula in the pulsar vicinity,which can be interpreted as jets bent by the ram pressure. The size of thiscompact part is about 30'', and it is surrounded by a weak asymmetric diffusiveemission extended up to $\approx$ 2.8'. The X-ray spectra of the pulsar, thecompact and extended parts of the nebula can be described by the power-lawmodels with photon indexes of 0.44, 2.34 and 2.14, respectively. The actualpulsar's X-ray flux is several times weaker than it was obtained with Suzakuand Swift where it was dominated by the unresolved nebula. We discuss possibleassociations of J1932+1916 with the nearby supernova remnant G54.4-0.3.

Studying the $\gamma$-ray pulsar J1932+1916 and its pulsar wind nebula with Chandra