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Issue A&A
Volume 448, Number 3, March IV 2006
Page(s) 817 - 822
Section Astrophysical processes
DOI http://dx.doi.org/10.1051/0004-6361:20053228

A&A 448, 817-822 (2006)
DOI: 10.1051/0004-6361:20053228

The iron K-shell features of MXB 1728-34 from a simultaneous Chandra-RXTE observation

A. D'Aí1, T. Di Salvo1, R. Iaria1, M. Méndez2, L. Burderi3, G. Lavagetto1, W. H. G. Lewin4, N. R. Robba1, L. Stella3 and M. van der Klis5

1  Dipartimento di Scienze Fisiche ed Astronomiche, Università di Palermo, via Archirafi 36, 90123 Palermo, Italy
    e-mail: dai@fisica.unipa.it
2  National Institute for Space Research, Sorbonnelaan 2, 3584 CA Utrecht, The Netherlands
3  Osservatorio Astronomico di Roma, via Frascati 33, 00040 Monteporzio Catone (Roma), Italy
4  Center for Space Research and Department of Physics, Massachusetts Institute of Technology, 70 Vassar Street, Cambridge, MA 02139, USA
5  Astronomical Institute "Anton Pannekoek", University of Amsterdam and Center for High-Energy Astrophysics, Kruislaan 403, 1098 SJ Amsterdam, The Netherlands

(Received 12 April 2005 / Accepted 28 October 2005)

Abstract
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 ( ${\it FWHM} \simeq 2$ 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 emission lines between 6 and 7 keV. We test our alternative model 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.


Key words: accretion, accretion disks -- stars: individual: MXB 1728-34 -- stars: neutron -- X-rays: stars -- X-rays: binaries -- X-rays: general

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© ESO 2006


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