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We analyze the ASCA spectrum of the Cen X-3 X-ray binary system in eclipseusing atomic models appropriate to recombination-dominated level populationkinetics in an overionized plasma. In order to estimate the windcharacteristics, we first fit the eclipse spectrum to a single-zonephotoionized plasma model. We then fit spectra from a range of orbital phasesusing global models of photoionized winds from the companion star and theaccretion disk that account for the continuous distribution of density andionization state. We find that the spectrum can be reproduced by a densitydistribution of the form derived by Castor, Abbot, & Klein (1975) forradiation-driven winds with with the value of the mass-loss rate divided by theterminal velocity consistent with values for isolated stars of the same stellartype. This is surprising because the neutron star is very luminous (~10^38erg/s) and the X-rays from the neutron star should ionize the wind and destroythe ions that provide the opacity for the radiation-driven wind. Using the samefunctional form for the density profile, we also fit the spectrum to aspherically symmetric wind centered on the neutron star, a configuration chosento represent a disk wind. We argue that the relatively modest orbital variationof the discrete spectrum rules out a disk wind hypothesis.Comment: ApJ accepte

The X‐Ray Photoionized Wind in Cen X‐3/V779 Cen