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The Korean Astronomical Society (한국천문학회)
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THE UPDATED ORBITAL PERIOD OF LOW MASS X-ray BINARY 4U 1323-62

  • CHUANG, PO-SHENG (Graduate Institute of Astromony, National Central University) ;
  • CHOU, YI (Graduate Institute of Astromony, National Central University) ;
  • HU, CHIN-PING (Graduate Institute of Astromony, National Central University) ;
  • YANG, TING-CHANG (Graduate Institute of Astromony, National Central University) ;
  • SU, YI-HAO (Graduate Institute of Astromony, National Central University) ;
  • LIAO, NAI-HUI (Graduate Institute of Astromony, National Central University) ;
  • HSIEH, HUNG-EN (Graduate Institute of Astromony, National Central University) ;
  • LIN, CHING-PING (Graduate Institute of Astromony, National Central University)
  • Received : 2014.11.30
  • Accepted : 2015.06.30
  • Published : 2015.09.30
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Abstract

4U 1323-62, a low mass X-ray binary with an orbital period of 2.94 hr, exhibits periodic X-ray dips, which are due to absorption by the bulge of the outer accretion disk. The purpose of this study is to search for orbital period changes using archived X-ray data over a time span of 20 years. We present our preliminary results from analyzing light curves observed by RXTE, BeppoSAX, XMM-Newton and Suzaku. We used the method proposed by Hu et al. (2008) to estimate dip center time and adopted the Observed - Calculated method to measure changes in period. We obtained an orbital period of 2.941917(36) hr and a period derivative of $\dot{P}_{orb}/P_{orb}=(-9.9{\pm}3.5){\times}10^{-7}yr^{-1}$. The F-test result shows that the quadratic ephemeris is describes the evolution of the dip phases better than the linear ephemeris at a greater than 95% confidence level. More X-ray data collected from the early 80s will be included to further refine the orbital ephemeris.

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References

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