Properties of X-ray binaries in the Magellanic Clouds from <i>RXTE</i> and <i>Chandra</i> observations

Corbet, R. H. D.; Coe, M. J.; McGowan, K.; Schurch, M. P. E.; Townsend, L. J.; Galache, J. L.; Marshall, F. E.

doi:10.1017/s1743921308028718

Cited by 10 publications

(6 citation statements)

References 9 publications

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“…The temporal separation of these outbursts suggests an orbital period of P o ∼ (146 ± 2) d, however this needs further confirmation. We note that this orbital period is in agreement with the spin period, according to the Corbet relation (Corbet 1984;Laycock et al 2005;Corbet et al 2009). …”

Section: Periodicitiessupporting

confidence: 85%

Discovery of SXP 265, a Be/X-ray binary pulsar in the Wing of the Small Magellanic Cloud★

Sturm

Haberl

Vasilopoulos

et al. 2014

Monthly Notices of the Royal Astronomical Society

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We identify a new candidate for a Be/X-ray binary in the XMM-Newton slew survey and archival Swift observations that is located in the transition region of the Wing of the Small Magellanic Cloud and the Magellanic Bridge. We investigated and classified this source with follow-up XMM-Newton and optical observations. We model the X-ray spectra and search for periodicities and variability in the X-ray observations and the OGLE I-band light curve. The optical counterpart has been classified spectroscopically, with data obtained at the SAAO 1.9 m telescope, and photometrically, with data obtained using GROND at the MPG 2.2 m telescope. The X-ray spectrum is typical of a high-mass X-ray binary with an accreting neutron star. We detect X-ray pulsations, which reveal a neutron-star spin period of P s = (264.516 ± 0.014) s. The source likely shows a persistent X-ray luminosity of a few 10 35 erg s −1 and in addition type-I outbursts that indicate an orbital period of ∼146 d. A periodicity of 0.867 d, found in the optical light curve, can be explained by non-radial pulsations of the Be star. We identify the optical counterpart and classify it as a B1-2II-IVe star. This confirms SXP 265 as a new Be/X-ray binary pulsar originating in the tidal structure between the Magellanic Clouds.

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Section: Periodicitiessupporting

confidence: 85%

Discovery of SXP 265, a Be/X-ray binary pulsar in the Wing of the Small Magellanic Cloud★

Sturm

Haberl

Vasilopoulos

et al. 2014

Monthly Notices of the Royal Astronomical Society

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“…The Type I outbursts occur periodically at the time of the periastron passage of the neutron star, whereas Type II outbursts are much more extensive and occur when the circumstellar material expands to fill most, or all of the orbit. General reviews of such HMXB systems may be found in Reig (2011), Negueruela (1998), Corbet et al (2009) and Coe et al (2000Coe et al ( , 2009.…”

Section: Introductionmentioning

confidence: 99%

SXP 5.05 = IGR J00569-7226: using X-rays to explore the structure of a Be star's circumstellar disc

Coe

Bartlett

Bird

et al. 2015

Monthly Notices of the Royal Astronomical Society

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On MJD 56590-1 (2013 Oct 25-26) observations of the Magellanic Clouds by the INTErnational Gamma-Ray Astrophysics Laboratory (INTEGRAL) observatory discovered a previously-unreported bright, flaring X-ray source. This source was initially given the identification IGR J00569-7226. Subsequent multi-wavelength observations identified the system as new Be/X-ray binary system in the Small Magellanic Cloud. Follow-up X-ray observations by Swift and XMM-Newton revealed an X-ray pulse period of 5.05s and that the system underwent regular occulation/eclipse behaviour every 17d. This is the first reported eclipsing Be/X-ray binary system in the SMC, and only the second such system known to date. Furthermore, the nature of the occultation makes it possible to use the neutron star to "X-ray" the circumstellar disk, thereby, for the first time, revealing direct observational evidence for its size and clumpy structure. Swift timing measurements allowed for the binary solution to be calculated from the Doppler shifted X-ray pulsations. This solution suggests this is a low eccentricity binary relative to others measured in the SMC. Finally it is interesting to note that the mass determined from this dynamical method for the Be star (∼ 13.0M ⊙ ) is significantly different from that inferred from the spectroscopic classification of B0.2Ve (∼ 16.0M ⊙ ) -an effect that has been noted for some other high mass X-ray binary (HMXB) systems.

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“…However, we would expect to observe a giant burst for a long recurrence interval (type II, >10 37 erg s −1 ; Caballero et al 2008). On the other hand, if the orbital period for 1A 1118−615 is 17 yr, this binary system will have the longest orbital period than all the other known Be/XBPs shown by Corbet et al (2009).…”

Section: Discussionmentioning

confidence: 94%

Swift observations of the Be/X-ray transient system 1A 1118−615

Lin

Takata

Kong

et al. 2010

Monthly Notices of the Royal Astronomical Society

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We report results of Swift observations for the high‐mass Be/X‐ray binary system 1A 1118−615, during an outburst stage in 2009 January and at a flaring stage in 2009 March. Using the epoch‐folding method, we successfully detected a pulsed period of 407.69(2) s in the outburst of January and of 407.26(1) s after the flare detection in March. We find that the spectral detection for the source during outburst can be described by a blackbody model with a high temperature () and a small radius ( km), indicating that the emission results from the polar cap of the neutron star. On the other hand, the spectra obtained after the outburst can further be described by adding an additional component with a lower temperature () and a larger emission radius ( km), which indicates the emission from around the inner region of an accretion disc. We find that the thermal emission from the hotspot of the accreting neutron star dominates the radiation in outburst; the existence of both this X‐ray contribution and the additional soft component suggests that the polar cap and the accretion disc emission might co‐exist after the outburst. Because the two‐blackbody signature at the flaring stage is a unique feature of 1A 1118−615, our spectral results may provide a new insight to interpret the X‐ray emission for the accreting neutron star. The time separation between the three main outbursts of this system is ∼17 yr and it might be related to the orbital period. We derive and discuss the associated physical properties by assuming the elongated orbit for this specific Be/X‐ray transient.

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Properties of X-ray binaries in the Magellanic Clouds from RXTE and Chandra observations

Cited by 10 publications

References 9 publications

Discovery of SXP 265, a Be/X-ray binary pulsar in the Wing of the Small Magellanic Cloud★

Discovery of SXP 265, a Be/X-ray binary pulsar in the Wing of the Small Magellanic Cloud★

SXP 5.05 = IGR J00569-7226: using X-rays to explore the structure of a Be star's circumstellar disc

Swift observations of the Be/X-ray transient system 1A 1118−615

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