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Spin period evolution of GX 1+4
Stockholm University, Faculty of Science, Department of Astronomy. Stockholm University, Faculty of Science, The Oskar Klein Centre for Cosmo Particle Physics (OKC).ORCID iD: 0000-0003-0716-107X
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Number of Authors: 72012 (English)In: Astronomy and Astrophysics, ISSN 0004-6361, E-ISSN 1432-0746, Vol. 537, article id A66Article in journal (Refereed) Published
Abstract [en]

Aims. We aim both to complement the existing data on the spin history of the peculiar accreting X-ray pulsar GX 1+4 with more past and current data from BeppoSAX, INTEGRAL, and Fermi and to interpret the evolution in the framework of accretion theory.

Methods. We used source light curves obtained from BeppoSAX/WFC and INTEGRAL/ISGRI to derive pulse periods using an epoch-folding analysis. Fermi/GBM data were analysed by fitting a constant plus a Fourier expansion to background-subtracted rates, and maximizing the Y-2 statistic. We completed the sample with hard X-ray light curves from Swift/BAT. The data were checked for correlations between flux and changes of the pulsar spin on different timescales.

Results. The spin-down of the pulsar continues with a constant change in frequency, i.e., an apparently accelerating change in the period. Over the past three decades, the pulse period has increased by about similar to 50%. Short-term fluctuations on top of this long-term trend do show anti-correlation with the source flux. Possible explanations of the observed long-term frequency and its dependence on flux are discussed.

Place, publisher, year, edition, pages
2012. Vol. 537, article id A66
Keywords [en]
accretion, accretion disks, X-rays: bursts, pulsars: individual: GX 1+4
National Category
Physical Sciences
Identifiers
URN: urn:nbn:se:su:diva-162450DOI: 10.1051/0004-6361/201117893ISI: 000300416800066OAI: oai:DiVA.org:su-162450DiVA, id: diva2:1267592
Available from: 2018-12-03 Created: 2018-12-03 Last updated: 2018-12-03Bibliographically approved

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Kretschmar, P.Larsson, StefanPostnov, K.
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