Swift/XRT monitoring of the Supergiant Fast X-ray Transient IGR J18483-0311 for an entire orbital period
arXiv:0909.5109 · doi:10.1111/j.1365-2966.2009.15789.x
Abstract
IGR J18483-0311 is an X-ray pulsar with transient X-ray activity, belonging to the new class of High Mass X-ray Binaries called Supergiant Fast X-ray Transients. This system is one of the two members of this class, together with IGR J11215-5952, where both the orbital (18.52d) and spin period (21s) are known. We report on the first complete monitoring of the X-ray activity along an entire orbital period of a Supergiant Fast X-ray Transient. These Swift observations, lasting 28d, cover more than one entire orbital phase consecutively. They are a unique data-set, which allows us to constrain the different mechanisms proposed to explain the nature of this new class of X-ray transients. We applied the new clumpy wind model for blue supergiants developed by Ducci et al. (2009), to the observed X-ray light curve. Assuming an eccentricity of e=0.4, the X-ray emission from this source can be explained in terms of the accretion from a spherically symmetric clumpy wind, composed of clumps with different masses, ranging from 10^{18}g to 5x 10^{21}g.
Accepted for publication in MNRAS. 7 pages, 7 figures, 2 tables
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- Seven Years with the Swift Supergiant Fast X-ray Transients Project
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- Astrophysical parameters and orbital solution of the peculiar X-ray transient IGR J00370+6122
- On More Sensitive Periodogram Statistics
- INTEGRAL discovery of unusually long broad-band X-ray activity from the Supergiant Fast X-ray Transient IGR J18483-0311
- The 100-month Swift catalogue of supergiant fast X-ray transients II. SFXT diagnostics from outburst properties
- X-ray irradiation of the stellar wind in HMXBs with B supergiants: Implications for ULXs