On the geometry of the X-ray emission from pulsars: the changing aspect of the Be/X-ray pulsar SXP348

• Published in: Monthly notices of the Royal Astronomical Society Vol. 486; no. 3; pp. 3248 - 3258
• Main Authors: Cappallo, R, Laycock, S G T, Christodoulou, D M, Coe, M J, Zezas, A
• Format: Journal Article
• Language: English
• Published: 01-07-2019
• ISSN: 0035-8711; 1365-2966
• DOI: 10.1093/mnras/stz1087

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.