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We present a statistical study of the non-thermal X-ray emission of 27 youngrotation powered pulsars (RPPs) and 24 pulsar wind nebulae (PWNe) by using theChandra and the XMM-Newton observations, which with the high spatialresolutions enable us to spatially resolve pulsars from their surrounding PWNe.We obtain the X-ray luminosities and spectra separately for RPPs and PWNe, andthen investigate their distribution and relation to each other as well as therelation with the pulsar rotational parameters. In the pair-correlationanalysis we find that: (1) the X-ray (2-10 keV) luminosities of both pulsar andPWN (L_{psr} and L_{pwn}) display a strong correlation with pulsar spin downpower Edot and characteristic age, and the scalings resulting from a simplelinear fit to the data are L_{psr} \propto Edot^{0.92 \pm 0.04} and L_{pwn}\propto Edot^{1.45 \pm 0.08} (68% confidence level), respectively, however,both the fits are not statistically acceptable; (2) L_{psr} also shows apossible weak correlation with pulsar period P and period derivative Pdot,whereas L_{pwn} manifests a similar weak correlation with Pdot only; (3) ThePWN photon index Gamma_{pwn} is positively correlated with L_{pwn} andL_{pwn}/Edot. We also found that the PWN X-ray luminosity is typically 1 to 10times larger than that from the underlying pulsar, and the PWN photon indicesspan a range of ~1.5 to ~2. The statistic study of PWN spectral propertiessupports the particle wind model in which the X-ray emitting electrons areaccelerated by the termination shock of the wind.

Non-Thermal X-ray Properties of Rotation Powered Pulsars and Their Wind Nebulae