RXTE and Swift Observations of SWIFT J0513.4-6547

Sahiner, S.
Serim, Muhammed Miraç
Baykal, Altan
We present timing and spectral analysis of Swift-XRT (X-ray Telescope) and RXTE-PCA (Rossi X-ray Timing Explorer-proportional Counter Array) observations of the transient Be/X-ray pulsar SWIFT J0513.4-6547 during its outburst in 2009 and its rebrightening in 2014. From 2009 observations, short-term spin-up rate of the source after the peak of the outburst is found to have about half of the value measured at the peak of the outburst by Coe et al. When the source is quiescent between 2009 and 2014, average spin-down rate of the source is measured to be similar to 1.52 x 10(-12) Hz s(-1) indicating a surface dipole magnetic field of similar to 1.5 x 10(13) G assuming a propeller state. From 2014 observations, short-term spin-down rate of the source is measured to be about two orders smaller than this long-term spin-down rate. The orbit of the source is found to be circular which is atypical for transient Be/X-ray binary systems. Hardness ratios of the source correlate with the X-ray luminosity up to 8.4 x 10(36) erg s(-1) in the 3-10 keV band, whereas for higher luminosities hardness ratios remain constant. Pulsed fractions are found to be correlated with the source flux. Overall Swift-XRT and RXTE-PCA energy spectrum of the source fit equally well to a model consisting of blackbody and power law, and a model consisting of a power law with high-energy cut-off. From the pulse phase-resolved spectra and pulse phase-resolved hardness ratios obtained using RXTE-PCA, it is shown that spectrum is softer for the phases between the two peaks of the pulse.


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İNAM, SITKI ÇAĞDAŞ; Townsend, L. J.; McBride, V. A.; Baykal, Altan; Coe, M. J.; Corbet, R. H. D. (Oxford University Press (OUP), 2009-05-21)
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 i...
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We probe the properties of the transient X-ray pulsar MAXI J1409-619 through RXTE and Swift follow-up observations of the outburst in 2010. We are able to phase-connect the pulse arrival times for the 25 d episode during the outburst. We suggest that either an orbital model (with P-orb similar or equal to 14.7(4) d) or a noise process due to random torque fluctuations (with S-r approximate to 1.3 x 10(-18) Hz(2) S-2 Hz(-1)) is plausible to describe the residuals of the timing solution. The frequency derivat...
Frequency-resolved spectroscopy of XB1323-619 using XMM-Newton data: detection of a reflection region in the disc
Balman, Şölen (Oxford University Press (OUP), 2010-09-21)
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Optical imaging and spectroscopic observation of the galactic supernova remnant G85.9-0.6
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Optical CCD imaging with H alpha and [SII] filters and spectroscopic observations of the galactic supernova remnant G85.9-0.6 have been performed for the first time. The CCD image data are taken with the 1.5 m Russian-Turkish Telescope (RTT150) at TBA degrees TAK National Observatory (TUG) and spectral data are taken with the Bok 2.3 m telescope on Kitt Peak, AZ.
Citation Formats
S. Sahiner, M. M. Serim, A. Baykal, and S. Ç. İNAM, “RXTE and Swift Observations of SWIFT J0513.4-6547,” MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY, pp. 845–852, 2016, Accessed: 00, 2020. [Online]. Available: https://hdl.handle.net/11511/42063.