X-ray flux related timing and spectral features of 2S 1417-62

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Inam S., Baykal A. , Scott D., Finger M., Swank J.

MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY, vol.349, no.1, pp.173-180, 2004 (Journal Indexed in SCI) identifier identifier

  • Publication Type: Article / Article
  • Volume: 349 Issue: 1
  • Publication Date: 2004
  • Doi Number: 10.1111/j.1365-2966.2004.07478.x
  • Page Numbers: pp.173-180
  • Keywords: accretion, accretion discs, stars : emission-line, Be, stars : neutron, X-rays : binaries, X-rays : individual : 2S 1417-62, PULSE FREQUENCY CHANGES, TRANSIENT, ACCRETION, EMISSION, STARS, ATMOSPHERES, PERFORMANCE, PULSATIONS, LUMINOSITY, DISCOVERY


Rossi X-ray Timing Explorer (RXTE) observations of the X-ray transient pulsar 2S 1417-62 between 1999 November and 2000 August with a total exposure of similar to394 ks have been analysed. Observations include a main outburst followed by a series of mini outbursts. Changes in pulse morphology and pulse fraction were found to be related to the changes in X-ray flux. Particularly low X-ray flux regions were found to have significantly lower pulse fractions with different pulse morphologies. The 3-60 keV Proportional Counter Array (PCA) High-Energy X-ray Timing Experiment (HEXTE) main outburst spectrum was modelled with an absorbed power-law model with high-energy cut-off and a Gaussian iron line complex feature. Using the same spectral model, individual 3-20 keV PCA spectra were found to be softer and less absorbed in low X-ray flux regions between outbursts. Spectral studies showed that hydrogen column density was correlated, and the power-law index was anticorrelated with the 3-20 keV X-ray flux. X-ray flux related spectral and timing features in 2S 1417 62, except for low X-ray flux regions, were interpreted as a sign of disc accretion with a similar accretion geometry with a varying mass accretion rate ((M)over dot), whereas spectral and timing features of the low X-ray flux regions were interpreted as a sign of possible temporary accretion geometry change prior to the next periastron where (M)over dot increases again to restore the original accretion geometry.