  We report on spectral and intensity variability analysis from a
Chandra/ACIS-S observation of the transient, type-I X-ray bursting low-mass
X-ray binary Cen X-4. The quiescent X-ray spectrum during this observation is
statistically identical to one observed previously with Beppo/SAX, and close,
but not identical, to one observed previously with ASCA. The X-ray spectrum is
best described as a pure Hydrogen atmosphere thermal spectrum plus a power-law
component that dominates the spectrum above 2 keV. The best-fit radius of the
neutron star is r=12.9+/-2.6 (d/1.2 kpc) km if the interstellar absorption is
fixed at the value implied by the optical reddening. Allowing the interstellar
absorption to be a free parameter yields r=19+45-10 (d/1.2 kpc) km (90%
confidence). The thermal spectrum from the neutron star surface is inconsistent
with a solar metallicity. We find a 3sigma upper-limit of root-mean-square
variability <18% (0.2-2.0 keV; 0.0001-1 Hz) during the observation. On the
other hand, the 0.5-10.0 keV luminosity decreased by 40+/-8% in the 4.9 years
between the Asca and Chandra observations. This variability can be attributed
to the power-law component. Moreover, we limit the variation in thermal
temperature to <10% over these 4.9 years. The stability of the thermal
temperature and emission area radius supports the interpretation that the
quiescent thermal emission is due to the hot neutron star core.
