6533b86dfe1ef96bd12ca03d
RESEARCH PRODUCT
The iron K-shell features of MXB 1728-34 from a simultaneous Chandra-RXTE observation
T. Di SalvoMariano MéndezR. IariaAntonino D'aiG. LavagettoN. R. RobbaLuciano BurderiLuigi StellaWalter H. G. LewinM. Van Der Klissubject
PhysicsAstrophysics::High Energy Astrophysical Phenomenaindividual : MXB 1728-34; stars : neutron; X-rays : stars; X-rays : binaries; X-rays : general [accretion accretion disks; stars]Astrophysics (astro-ph)X-ray binaryElectron shellAstronomyFOS: Physical sciencesAstronomy and AstrophysicsAstrophysicsAstrophysicsaccretion accretion diskstars : neutronNeutron starAbsorption edgeSpace and Planetary ScienceIonizationX-rays : starBlack-body radiationEmission spectrumBasso continuoX-rays : binariestars : individual : MXB 1728-34X-rays : generaldescription
We report on a simultaneous Chandra and RossiXTE observation of the low-mass X-ray binary atoll bursting source MXB 1728-34 performed on 2002 March 3-5. We fit the 1.2-35 keV continuum spectrum with a blackbody plus a Comptonized component. Large residuals at 6-10 keV can be fitted by a broad (FWHM ~ 2 keV) Gaussian emission line or, alternatively, by two absorption edges associated with lowly ionized iron and Fe XXV/XXVI at ~7.1 keV and ~9 keV, respectively. In this interpretation, we find no evidence of broad, or narrow, emission lines between 6 and 7 keV. We test our alternative modelling of the iron K shell region by reanalysing a previous BeppoSAX observation of MXB 1728-34, finding a general agreement with our new spectral model.
| year | journal | country | edition | language |
|---|---|---|---|---|
| 2005-11-02 |