C.D.S. - SIMBAD4 rel 1.7 - 2020.09.18CEST10:03:33

2001A&A...376..532O - Astronomy and Astrophysics, volume 376, 532-542 (2001/9-3)

BeppoSAX observation of the eclipsing dipping X-ray binary X1658-298.


Abstract (from CDS):

Result. of a 2000 August 12-13 BeppoSAX observation of the 7.1 hr eclipsing, dipping, bursting, transient, low-mass X-ray binary (LMXRB) X1658-298 are presented. The spectrum outside of eclipses, dips and bursts can be modeled by the combination of a soft disk-blackbody and a harder Comptonized component with a small amount (1.3x1021atom/cm2) of low-energy absorption. In contrast, an RXTE observation 18 months earlier during the same outburst, measured an absorption of 5.0x1022atom/cm2. Such a change is consistent with a thinning of the accretion disk as the outburst progresses. Structured residuals from the best-fit spectral model are present which are tentatively identified with Ne-K/Fe-L and Fe-K shell emission. The spectral changes during dips are complex and may be modeled by a strong (∼3x1023atom/cm2) increase in absorption of the Comptonized component only, together with reductions in normalizations of both spectral components. This behavior is in contrast to the ``complex continuum'' model for X-ray dip sources, where the softer blackbody component rapidly suffers strong absorption. It is however, similar to that found during recent XMM-Newton observations of the eclipsing, dipping, LMXRB EXO0748-676. An updated orbital ephemeris is provided which does not require a quadratic term, in contrast to that of Wachter et al. (2000ApJ...534..367W).

Abstract Copyright:

Journal keyword(s): accretion, accretion disks - stars: individual: X1658-298 - stars: neutron - X-rays: stars

Simbad objects: 2

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Number of rows : 2

N Identifier Otype ICRS (J2000)
ICRS (J2000)
Mag U Mag B Mag V Mag R Mag I Sp type #ref
1850 - 2020
1 V* UY Vol LXB 07 48 33.71 -67 45 07.7 16.10 17.00 16.9 16.7 17.05 ~ 574 0
2 MXB 1658-298 LXB 17 02 06.54 -29 56 44.1 18.35 18.75 18.3     ~ 326 0

    Equat.    Gal    SGal    Ecl

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