An XMM-Newton study of the X-ray binary MXB 1659-298 and the discovery of narrow X-ray absorption lines

Free access article

Issue		A&A Volume 379, Number 2, November IV 2001


Page(s)		540 - 550
Section		Formation, structure and evolution of stars
DOI		http://dx.doi.org/10.1051/0004-6361:20011322

A&A 379, 540-550 (2001)
DOI: 10.1051/0004-6361:20011322

An XMM-Newton study of the X-ray binary MXB 1659-298 and the discovery of narrow X-ray absorption lines

L. Sidoli, T. Oosterbroek, A. N. Parmar, D. Lumb and C. Erd

Space Science Department of ESA, ESTEC, Postbus 299, 2200 AG Noordwijk, The Netherlands

(Received 23 July 2001 / Accepted 17 September 2001 )

Abstract
We report the discovery of narrow X-ray absorption lines from the low-mass X-ray binary MXB 1659-298 during an XMM-Newton observation in 2001 February. The 7.1 hr orbital cycle is clearly evident with narrow X-ray eclipses preceded by intense dipping activity. A sinusoid-like OM B-band modulation with a peak-to-peak modulation of ~0.5 mag and a minimum coincident with the X-ray eclipse is visible. EPIC and RGS spectra reveal the presence of narrow resonant absorption features identified with O VIII 1s-2p, 1s-3p and 1s-4p, Ne X 1s-2p, Fe XXV 1s-2p, and Fe XXVI 1s-2p transitions, together with a broad Fe emission feature at 6.47 ^+0.18 _-0.14 keV. The equivalent widths of the Fe absorption features show no obvious dependence on orbital phase, even during dipping intervals. The equivalent widths of the other features are consistent with having the same values during persistent and dipping intervals. Previously, the only X-ray binaries known to exhibit narrow X-ray absorption lines were two superluminal jet sources and it had been suggested that these features are related to the jet formation mechanism. This now appears unlikely, and instead their presence may be related to the viewing angle of the system. The MXB 1659-298 0.6-12 keV continuum is modeled using absorbed cutoff power-law and blackbody components. During dips the blackbody is more strongly absorbed than the power-law. The spectral shape of the 3.6% of 0.5-10 keV emission that remains during eclipses is consistent with that during non-dipping intervals.

Key words: accretion, accretion disks -- stars: individual: MXB 1659-298 -- stars: neutron -- X-rays: general

Offprint request: L. Sidoli, sidoli@ifctr.mi.cnr.it

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