Please use this identifier to cite or link to this item: http://hdl.handle.net/2381/40363
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dc.contributor.authorTownsend, L. J.-
dc.contributor.authorKennea, J. A.-
dc.contributor.authorCoe, M. J.-
dc.contributor.authorMcBride, V. A.-
dc.contributor.authorBuckley, D. A. H.-
dc.contributor.authorEvans, Philip Andrew-
dc.contributor.authorUdalski, A.-
dc.date.accessioned2017-09-12T14:34:55Z-
dc.date.available2017-09-12T14:34:55Z-
dc.date.issued2017-07-25-
dc.identifier.citationMonthly Notices of the Royal Astronomical Society, 2017, 471 (11), pp. 3878-3887en
dc.identifier.issn0035-8711-
dc.identifier.urihttps://academic.oup.com/mnras/article/471/4/3878/4035916/The-2016-superEddington-outburst-of-SMC-X3-Xrayen
dc.identifier.urihttp://hdl.handle.net/2381/40363-
dc.description.abstractOn 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.en
dc.language.isoenen
dc.publisherOxford University Press on behalf of the Royal Astronomical Societyen
dc.relation.urihttp://arxiv.org/abs/1701.02336v2-
dc.rightsCopyright © 2017 The Author(s). Deposited with reference to the publisher’s open access archiving policy.en
dc.subjectastro-ph.HEen
dc.subjectastro-ph.HEen
dc.titleThe 2016 super-Eddington outburst of SMC X-3: X-ray and optical properties and system parametersen
dc.typeJournal Articleen
dc.identifier.doi10.1093/mnras/stx1865-
dc.identifier.eissn1365-2966-
dc.description.statusPeer-revieweden
dc.description.versionPublisher Versionen
pubs.organisational-group/Organisationen
pubs.organisational-group/Organisation/COLLEGE OF SCIENCE AND ENGINEERINGen
pubs.organisational-group/Organisation/COLLEGE OF SCIENCE AND ENGINEERING/Department of Physics and Astronomyen
dc.dateaccepted2017-07-20-
Appears in Collections:Published Articles, Dept. of Physics and Astronomy

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