The quiescent X-ray spectrum of the neutron star in Centaurus X-4 observedwith Chandra/ACIS-S

We report on spectral and intensity variability analysis from a Chandra/ACI S-S observation of the transient, type I X-ray bursting low-mass X-ray bina ry Cen X-4. The quiescent X-ray spectrum during this observation is statist ically identical to one observed previously with BeppoSAX and close, but no t identical, to one observed previously with ASCA. The X-ray spectrum is be st described as a pure hydrogen atmosphere thermal spectrum plus a power-la w 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 ab sorption is fixed at the value implied by the optical reddening. Allowing t he interstellar absorption to be a free parameter yields r = 19(-10)(+45) ( d/1.2 kpc) km (90% confidence). The thermal spectrum from the neutron star surface is inconsistent with a solar metallicity. We find a 3 sigma upper l imit of rms variability less than or equal to 18% (0.2-2.0 keV; 0.0001-1 Hz ) during the observation. On the other hand, the 0.5-10.0 keV luminosity de creased by 40 +/- 8% in the 4.9 yr between the ASCA and Chandra observation s. This variability can be attributed to the power-law component. Moreover, we limit the variation in thermal temperature to less than or similar to 1 0% over these 4.9 yr. The stability of the thermal temperature and emission -area radius supports the interpretation that the quiescent thermal emissio n is caused by the hot neutron star core.