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On the Geometry of the X-ray emission from pulsars a consistent inclination and beaming solution for the Be/X-ray pulsar SXP 1062

On the Geometry of the X-ray emission from pulsars a consistent inclination and beaming solution for the Be/X-ray pulsar SXP 1062
On the Geometry of the X-ray emission from pulsars a consistent inclination and beaming solution for the Be/X-ray pulsar SXP 1062
SXP 1062 is a long-period X-ray pulsar (XRP) with a Be optical companion located in the Small Magellanic Cloud. First discovered in 2010 from XMM–Newton data, it has been the target of multiple observational campaigns due to the seeming incongruity between its long spin period and recent birth. In our continuing modelling efforts to determine the inclination angle (i) and magnetic axis angle (θ) of XRPs, we have fitted 19 pulse profiles from SXP 1062 with our pulsar model, Polestar, including three consecutive Chandra observations taken during the trailing end of a Type I outburst. These fittings have resulted in most likely values of i = 76 ± 2 and θ = 40 ± 9. SXP 1062 mostly displays a stable double-peaked pulse profile with the peaks separated by roughly a third of a phase, but recently the pulsar has spun up and widened to a spacing of roughly half of a phase, yet the Polestar fits for i and θ remain constant. Additionally, we note a possible correlation between the X-ray luminosity and the separation of the peaks in the pulse profiles corresponding to the highest luminosity states.
0035-8711
2152–2161
Capallo, R.C.
9bab4f21-88ea-40c6-84b8-ab0573e26a03
Laycock, S.G.T.
dcc0a71c-272a-4f58-b4bb-69accffcf485
Christodoulou, D.M.
61b4aa30-c75b-4141-82f2-ae0466e22253
Roy, A.
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Bhattacharya, S.
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Coe, Malcolm
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Zezas, A.
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Capallo, R.C.
9bab4f21-88ea-40c6-84b8-ab0573e26a03
Laycock, S.G.T.
dcc0a71c-272a-4f58-b4bb-69accffcf485
Christodoulou, D.M.
61b4aa30-c75b-4141-82f2-ae0466e22253
Roy, A.
5571d417-c91b-425b-9fc0-98816c750d7a
Bhattacharya, S.
d06038bd-c92a-4838-a01d-3ab58eaa715a
Coe, Malcolm
04dfb23b-1456-46a3-9242-5cee983471d5
Zezas, A.
f6fb6477-2c0a-4688-9dbd-c53cfa3306fd

Capallo, R.C., Laycock, S.G.T., Christodoulou, D.M., Roy, A., Bhattacharya, S., Coe, Malcolm and Zezas, A. (2020) On the Geometry of the X-ray emission from pulsars a consistent inclination and beaming solution for the Be/X-ray pulsar SXP 1062. Monthly Notices of the Royal Astronomical Society, 495 (2), 2152–2161. (doi:10.1093/mnras/staa1320).

Record type: Article

Abstract

SXP 1062 is a long-period X-ray pulsar (XRP) with a Be optical companion located in the Small Magellanic Cloud. First discovered in 2010 from XMM–Newton data, it has been the target of multiple observational campaigns due to the seeming incongruity between its long spin period and recent birth. In our continuing modelling efforts to determine the inclination angle (i) and magnetic axis angle (θ) of XRPs, we have fitted 19 pulse profiles from SXP 1062 with our pulsar model, Polestar, including three consecutive Chandra observations taken during the trailing end of a Type I outburst. These fittings have resulted in most likely values of i = 76 ± 2 and θ = 40 ± 9. SXP 1062 mostly displays a stable double-peaked pulse profile with the peaks separated by roughly a third of a phase, but recently the pulsar has spun up and widened to a spacing of roughly half of a phase, yet the Polestar fits for i and θ remain constant. Additionally, we note a possible correlation between the X-ray luminosity and the separation of the peaks in the pulse profiles corresponding to the highest luminosity states.

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Accepted/In Press date: 7 May 2020
e-pub ahead of print date: 14 May 2020
Published date: June 2020

Identifiers

Local EPrints ID: 443056
URI: http://eprints.soton.ac.uk/id/eprint/443056
ISSN: 0035-8711
PURE UUID: 7a542185-5110-4280-bea9-2ea670f7bcac
ORCID for Malcolm Coe: ORCID iD orcid.org/0000-0002-0763-8547

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Date deposited: 07 Aug 2020 16:30
Last modified: 08 Aug 2020 01:31

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Contributors

Author: R.C. Capallo
Author: S.G.T. Laycock
Author: D.M. Christodoulou
Author: A. Roy
Author: S. Bhattacharya
Author: Malcolm Coe ORCID iD
Author: A. Zezas

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