RXTE-PCA Observations of XMMU J054134.7-682550
Abstract
We analyzed RXTE-PCA observations of a recent outburst of the X-ray pulsar XMMU J054134.7682550. 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.
Keywords
Cite
@article{arxiv.0810.0958,
title = {RXTE-PCA Observations of XMMU J054134.7-682550},
author = {S. C. Inam and L. J. Townsend and V. A. McBride and A. Baykal and M. J. Coe and R. H. D. Corbet},
journal= {arXiv preprint arXiv:0810.0958},
year = {2009}
}
Comments
Published in MNRAS