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|Title:||The 2016 super-Eddington outburst of SMC X-3: X-ray and optical properties and system parameters|
|Authors:||Townsend, L. J.|
Kennea, J. A.
Coe, M. J.
McBride, V. A.
Buckley, D. A. H.
Evans, Philip Andrew
|Publisher:||Oxford University Press on behalf of the Royal Astronomical Society|
|Citation:||Monthly Notices of the Royal Astronomical Society, 2017, 471 (11), pp. 3878-3887|
|Abstract:||On 2016 July 30 (MJD 57599), observations of the Small Magellanic Cloud by Swift/XRT found an increase in X-ray counts coming from a position consistent with the Be/X-ray binary pulsar SMC X-3. Follow-up observations on 2016 August 3 (MJD 57603) and 2016 August 10 (MJD 57610) revealed a rapidly increasing count rate and confirmed the onset of a new X-ray outburst from the system. Further monitoring by Swift began to uncover the enormity of the outburst, which peaked at 1.2 x 10^39 erg/s on 2016 August 25 (MJD 57625). The system then began a gradual decline in flux that was still continuing over 5 months after the initial detection. We explore the X-ray and optical behaviour of SMC X-3 between 2016 July 30 and 2016 December 18 during this super-Eddington outburst. We apply a binary model to the spin-period evolution that takes into account the complex accretion changes over the outburst, to solve for the orbital parameters. Our results show SMC X-3 to be a system with a moderately low eccentricity amongst the Be/X-ray binary systems and to have a dynamically determined orbital period statistically consistent with the prominent period measured in the OGLE optical light curve. Our optical and X-ray derived ephemerides show that the peak in optical flux occurs roughly 6 days after periastron. The measured increase in I-band flux from the counterpart during the outburst is reflected in the measured equivalent width of the H-alpha line emission, though the H-alpha emission itself seems variable on sub-day time-scales, possibly due to the NS interacting with an inhomogeneous disc.|
|Rights:||Copyright © 2017 The Author(s). Deposited with reference to the publisher’s open access archiving policy.|
|Appears in Collections:||Published Articles, Dept. of Physics and Astronomy|
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|MNRAS 471, 3878–3887 (2017).pdf||Published (publisher PDF)||1.11 MB||Adobe PDF||View/Open|
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