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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.

RXTE –PCA observations of XMMU J054134.7−682550