The Quiescent X-Ray Spectrum of the Neutron Star in Cen X-4 Observed with Chandra/ACIS-S

Details The Quiescent X-Ray Spectrum of the Neutron Star in Cen X-4 Observed with Chandra/ACIS-S The Quiescent X-Ray Spectrum of the Neutron Star in Cen X-4 Observed with Chandra/ACIS-S

2000-12-19

arxiv.org/abs/astro-ph/0012400v1

Astronomy and Astrophysics

Astrophysics

25 pages, 1 figure; ApJ, Accepted for April 10 2001 Issue

Scientific paper

10.1086/320247

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.

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