RXTE-PCA Observations of XMMU J054134.7-682550

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dc.creatorInam, S. C.
dc.creatorTownsend, L. J.
dc.creatorMcBride, V. A.
dc.creatorBaykal, A.
dc.creatorCoe, M. J.
dc.creatorCorbet, R. H. D.
dc.date2008-10-06
dc.date2009-05-15
dc.date.accessioned2026-07-07T13:14:46Z
dc.date.available2026-07-07T13:14:46Z
dc.descriptionWe analyzed RXTE-PCA observations of a recent outburst of the X-ray pulsar XMMU J054134.7$-$682550. We calculated the pulse frequency history of the source. We found no sign of a binary companion. The source spins up when the X-ray flux is higher, with a correlation between the spin-up rate and X-ray flux, which may be interpreted as a sign of an accretion disk. On the other hand, the source was found to have an almost constant spin frequency when the X-ray flux is lower without any clear sign of a spin-down episode. The decrease in pulsed fraction with decreasing X-ray flux was intrepreted as a sign of accretion geometry change, but we did not find any evidence of a transition from accretor to propeller regimes. The source was found to have variable pulse profiles. Two peaks in pulse profiles were usually observed. We studied the X-ray spectral evolution of the source throughout the observation. Pulse phase resolved analysis does not provide any further evidence for a cyclotron line, but may suggest a slight variation of intensity and width of the 6.4 keV iron line with phase.
dc.descriptionPublished in MNRAS
dc.identifierhttps://arxiv.org/abs/0810.0958
dc.identifierhttp://arxiv.org/abs/0810.0958
dc.identifier2009MNRAS.395.1662I
dc.identifierdoi:10.1111/j.1365-2966.2009.14659.x
dc.identifier.urihttp://salesiana.dossiersoluciones.com/handle/123456789/230282
dc.subjectAstrophysics
dc.titleRXTE-PCA Observations of XMMU J054134.7-682550
dc.typetext

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