Broad-band BeppoSAX observation of the low-mass X-ray binary X1822-371

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dc.creatorParmar, A. N.
dc.creatorOosterbroek, T.
dc.creatorDel Sordo, S.
dc.creatorSegreto, A.
dc.creatorSantangelo, A.
dc.creatorFiume, D. Dal
dc.creatorOrlandini, M.
dc.date2000-01-24
dc.date.accessioned2026-07-07T01:51:51Z
dc.date.available2026-07-07T01:51:51Z
dc.descriptionResults of a 1997 September 9-10 BeppoSAX observation of the 5.57 hr low-mass X-ray binary (LMXRB) X1822-371 are presented. The 0.3-40 keV spectrum is unusually complex and cannot be fit by any of the standard models applied to other LMXRB. At least two components are required. One component has a shape consistent with that expected from the Comptonization of an input soft (Wein) spectrum while the other, contributing ~40% of the 1-10 keV flux, is consistent with being a blackbody. In addition, there is a ``dip'' in the spectrum which can be modeled by a 1.33 +0.05 -0.11 keV absorption edge with an optical depth, tau, of 0.28 +/- 0.06. If the same model is fit to ASCA Solid-State Imaging Spectrometer spectra obtained in 1993 and 1996, then reasonable fits are also obtained, with a similar absorption feature required. The nature of this feature is highly uncertain; its energy corresponds to the K-edges of highly ionized Ne x and neutral Mg, or to an L-edge of moderately ionized Fe. Surprisingly, no strong (tau > 0.05) Fe-K or (tau > 0.18) O-K edges are visible. The folded lightcurve of X1822-371 is similar to previous observations, except that no strong softening is seen near the eclipse. An updated orbital ephemeris is provided.
dc.description7 pages. To appear in A&A
dc.identifierhttps://arxiv.org/abs/astro-ph/0001407
dc.identifierhttp://arxiv.org/abs/astro-ph/0001407
dc.identifier.urihttp://salesiana.dossiersoluciones.com/handle/123456789/436
dc.subjectAstrophysics
dc.titleBroad-band BeppoSAX observation of the low-mass X-ray binary X1822-371
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