  We 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.
