RXTE-PCA observations of XMMU J054134.7-682550


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İNAM S. Ç. , Townsend L. J. , McBride V. A. , BAYKAL A. , Coe M. J. , Corbet R. H. D.

MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY, cilt.395, ss.1662-1668, 2009 (SCI İndekslerine Giren Dergi) identifier identifier

  • Cilt numarası: 395 Konu: 3
  • Basım Tarihi: 2009
  • Doi Numarası: 10.1111/j.1365-2966.2009.14659.x
  • Dergi Adı: MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY
  • Sayfa Sayıları: ss.1662-1668

Özet

We analysed Rossi X-ray Timing Explorer Proportional Counter Array 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 disc. 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 interpreted 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.