On the geometry of the X-ray emission from pulsars: the changing aspect of the Be/X-ray pulsar SXP348
On the geometry of the X-ray emission from pulsars: the changing aspect of the Be/X-ray pulsar SXP348
The X-ray source SXP348 is a high-mass X-ray binary system in the Small Magellanic Cloud. Since its 1998 discovery by BeppoSAX, this pulsar has exhibited a spin period of 340 -350 s. In an effort to determine the orientation and magnetic geometry of this source, we used our geometric model Polestar to fit 71 separate pulse profiles extracted from archival Chandra and XMM-Newton observations over the past two decades. During 2002 pulsations ceased being detectable for nine months despite the source remaining in a bright state. When pulsations resumed, our model fits changed,
displaying a change in accretion geometry. Furthermore, in 2006 detectable pulsations again ceased, with 2011 marking the last positive detection of SXP348 as a point source. These profile fits will be released for public use as part of the database of Magellanic Cloud pulsars.
accretion and accretion discs, x-ray binary stars
3248-3258
Cappallo, R.
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Laycock, S.G.T.
3021ea8f-9d14-4cda-93cd-6776c37ed386
Christodoulou, D.
bc2ffc31-ee84-43a9-b941-8d22022f2d72
Coe, M.J.
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Zezas, A.
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Cappallo, R.
7f656c89-3406-46e3-9d11-87ed5b10fde3
Laycock, S.G.T.
3021ea8f-9d14-4cda-93cd-6776c37ed386
Christodoulou, D.
bc2ffc31-ee84-43a9-b941-8d22022f2d72
Coe, M.J.
04dfb23b-1456-46a3-9242-5cee983471d5
Zezas, A.
f6fb6477-2c0a-4688-9dbd-c53cfa3306fd
Cappallo, R., Laycock, S.G.T., Christodoulou, D., Coe, M.J. and Zezas, A.
(2019)
On the geometry of the X-ray emission from pulsars: the changing aspect of the Be/X-ray pulsar SXP348.
Monthly Notices of the Royal Astronomical Society, 486 (3), .
(doi:10.1093/mnras/stz1087).
Abstract
The X-ray source SXP348 is a high-mass X-ray binary system in the Small Magellanic Cloud. Since its 1998 discovery by BeppoSAX, this pulsar has exhibited a spin period of 340 -350 s. In an effort to determine the orientation and magnetic geometry of this source, we used our geometric model Polestar to fit 71 separate pulse profiles extracted from archival Chandra and XMM-Newton observations over the past two decades. During 2002 pulsations ceased being detectable for nine months despite the source remaining in a bright state. When pulsations resumed, our model fits changed,
displaying a change in accretion geometry. Furthermore, in 2006 detectable pulsations again ceased, with 2011 marking the last positive detection of SXP348 as a point source. These profile fits will be released for public use as part of the database of Magellanic Cloud pulsars.
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Accepted/In Press date: 11 April 2019
e-pub ahead of print date: 23 April 2019
Keywords:
accretion and accretion discs, x-ray binary stars
Identifiers
Local EPrints ID: 430465
URI: http://eprints.soton.ac.uk/id/eprint/430465
ISSN: 1365-2966
PURE UUID: cc885b98-e005-4de3-a5d7-2fe9e3f1a4d7
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Date deposited: 01 May 2019 16:30
Last modified: 10 Apr 2025 01:32
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Contributors
Author:
R. Cappallo
Author:
S.G.T. Laycock
Author:
D. Christodoulou
Author:
A. Zezas
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