Optical and X-ray study of the peculiar high mass X-ray binary XMMU J010331.7-730144

For a long time XMMU J010331.7-730144 was proposed as a high-mass X-ray binary candidate based on its X-ray properties, however, its optical behaviour was unclear - in particular previous observations did not reveal key Balmer emission lines. In this paper we report on optical and X-ray variability...

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Bibliographic Details
Published in:arXiv.org 2020-06
Main Authors: Monageng, Itumeleng M, Coe, Malcolm J, Buckley, David A H, McBride, Vanessa A, Kennea, Jamie A, Udalski, Andrzej, Evans, Phil A, J Simon Clark, Negueruela, Ignacio
Format: Article
Language:English
Subjects:
B stars
Companion stars
Deposition
Emission
Gravitational lenses
H alpha line
Neutron flux
Neutron stars
Optical properties
Outbursts
Variability
X ray binaries
X ray stars
X-rays
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Summary:For a long time XMMU J010331.7-730144 was proposed as a high-mass X-ray binary candidate based on its X-ray properties, however, its optical behaviour was unclear - in particular previous observations did not reveal key Balmer emission lines. In this paper we report on optical and X-ray variability of the system. XMMU J010331.7-730144 has been monitored with the Optical Gravitational Lensing Experiment (OGLE) in the I and V-bands for the past 9 years where it has shown extremely large amplitude outbursts separated by long periods of low-level flux. During its most recent optical outburst we obtained spectra with the Southern Africa Large Telescope (SALT) where, for the first time, the H-alpha line is seen in emission, confirming the Be nature of the optical companion. The OGLE colour-magnitude diagrams also exhibit a distinct loop which is explained by changes in mass-loss from the Be star and mass outflow in its disc. In the X-rays, XMMU J010331.7-730144 has been monitored by the Neil Gehrels Swift Observatory through the S-CUBED programme. The X-ray flux throughout the monitoring campaign shows relatively low values for a typical Be/X-ray binary system. We show, from the analysis of the optical data, that the variability is due to the Be disc density and opacity changing rather than its physical extent as a result of efficient truncation by the NS. The relatively low X-ray flux can then be explained by the neutron star normally accreting matter at a low rate due to the small radial extent of the Be disc.
ISSN:2331-8422
DOI:10.48550/arxiv.2006.07671