Evolution of high-mass X-ray binaries in the small magellanic cloud

2019 ◽  
Vol 340 (1-3) ◽  
pp. 46-49
Author(s):  
J. Yang ◽  
D. R. Wik ◽  
A. Zezas ◽  
S. G. T. Laycock ◽  
J. Hong ◽  
...  
Keyword(s):  
Magellanic Cloud ◽  
High Mass ◽  
Small Magellanic Cloud ◽  
X Ray ◽  
X Ray Binaries

scholarly journals Deep Chandra Survey of the Small Magellanic Cloud. III. Formation Efficiency of High-mass X-Ray Binaries

2019 ◽  
Vol 887 (1) ◽  
pp. 20 ◽  
Author(s):  
Vallia Antoniou ◽  
Andreas Zezas ◽  
Jeremy J. Drake ◽  
Carles Badenes ◽  
Frank Haberl ◽  
...  
Keyword(s):  
Magellanic Cloud ◽  
High Mass ◽  
Small Magellanic Cloud ◽  
X Ray ◽  
Formation Efficiency ◽  
X Ray Binaries

scholarly journals Evidence for Low Kick Velocities among High-mass X-Ray Binaries in the Small Magellanic Cloud from the Spatial Correlation Function

2021 ◽  
Vol 919 (2) ◽  
pp. 81
Author(s):  
Arash Bodaghee ◽  
Vallia Antoniou ◽  
Andreas Zezas ◽  
John A. Tomsick ◽  
Zachary Jordan ◽  
...  
Keyword(s):  
Correlation Function ◽  
Spatial Correlation ◽  
Magellanic Cloud ◽  
High Mass ◽  
Small Magellanic Cloud ◽  
Spatial Correlation Function ◽  
X Ray ◽  
X Ray Binaries

Evolution of High-mass X-ray binaries in the Small Magellanic Cloud

2018 ◽  
Vol 14 (S346) ◽  
pp. 353-357
Author(s):  
Jun Yang ◽  
Daniel R. Wik
Keyword(s):  
Neutron Star ◽  
Magellanic Cloud ◽  
High Mass ◽  
Small Magellanic Cloud ◽  
Third Body ◽  
X Ray ◽  
Spin Period ◽  
Period Derivative ◽  
X Ray Binaries ◽  
Small Period

AbstractIn order to understand the progenitor of rotation powered pulsars, we compare them with High-mass X-ray binary (HMXB) pulsars, (or X-ray pulsars), in the Small Magellanic Cloud. The plot of period period vs. period derivative shows that isolated neutron stars could be evolved from HMXBs. The pulsars with long spin period might spin up to 0.001-1 s. The mechanism is a third-body interaction that detaches the donor, leaving an isolated, small period neutron star behind.

scholarly journals Hα imaging for BeXRBs in the Small Magellanic Cloud

2016 ◽  
Vol 12 (S329) ◽  
pp. 373-375 ◽  
Author(s):  
G. Maravelias ◽  
A. Zezas ◽  
V. Antoniou ◽  
D. Hatzidimitriou ◽  
F. Haberl
Keyword(s):  
Narrow Band ◽  
Formation Rate ◽  
Broad Band ◽  
Magellanic Cloud ◽  
High Mass ◽  
Wide Field ◽  
Small Magellanic Cloud ◽  
X Ray ◽  
Hα Emission ◽  
X Ray Binaries

AbstractThe Small Magellanic Cloud (SMC) hosts a large number of high-mass X-ray binaries, and in particular of Be/X-ray Binaries (BeXRBs; neutron stars orbiting OBe-type stars), offering a unique laboratory to address the effect of metalicity. One key property of their optical companion is Hα in emission, which makes them bright sources when observed through a narrow-band Hα filter. We performed a survey of the SMC Bar and Wing regions using wide-field cameras (WFI@MPG/ESO and MOSAIC@CTIO/Blanco) in order to identify the counterparts of the sources detected in our XMM-Newton survey of the same area. We obtained broad-band R and narrow-band Hα photometry, and identified ~10000 Hα emission sources down to a sensitivity limit of 18.7 mag (equivalent to ~B8 type Main Sequence stars). We find the fraction of OBe/OB stars to be 13% down to this limit, and by investigating this fraction as a function of the brightness of the stars we deduce that Hα excess peaks at the O9-B2 spectral range. Using the most up-to-date numbers of SMC BeXRBs we find their fraction over their parent population to be ~0.002 − 0.025 BeXRBs/OBe, a direct measurement of their formation rate.

scholarly journals Confirmation of six Be X-ray binaries in the Small Magellanic Cloud

2017 ◽  
Vol 467 (2) ◽  
pp. 1526-1530 ◽  
Author(s):  
V. A. McBride ◽  
A. González-Galán ◽  
A. J. Bird ◽  
M. J. Coe ◽  
E. S. Bartlett ◽  
...  
Keyword(s):  
Magellanic Cloud ◽  
Small Magellanic Cloud ◽  
X Ray ◽  
X Ray Binaries
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