  We present high angular resolution X-ray images and spectra from two {\em
Chandra} ACIS-I observations of the X-ray jet in the nearby radio galaxy
Centaurus A. We find that the X-ray emission from the jet is composed of a low
surface brightness diffuse component extending continuously from within at
least 60 pc of the active nucleus into the NE radio lobe 4 kpc from the
nucleus, along with 31 discrete compact knots, most of which are extended at
the resolution of our observation. We find that there are small but significant
differences between the X-ray and radio morphologies of the inner jet at the
arcsecond level, making it unlikely that a single, spatially coincident
population of ultrarelativistic electrons is responsible for the emission in
both energy regimes. We suggest that the X-ray knots of the inner jet are
indeed the sites of particle acceleration and shocks, and the X-ray and radio
knot offsets are caused by a combination of particle diffusion and energy loss.
These offsets may be a common feature of all jets in radio galaxies, or at
least jets in FR I type galaxies, and may be fundamental to the physics of such
jets. The X-ray spectra of several regions of the jet are well fit by absorbed
power-law models with photon indices $\sim$2.2-2.5, although the spectrum of
one bright knot located $\sim$1 kpc from the nucleus (knot B) is harder (photon
index = 2.0).
