Cen X-3的准周期振荡和长期强度变化
Quasiperiodic oscillations in Cen X-3 and the long term intensity variations
摘要：
利用Rossi X射线定时探测器（\it {Rossi X-ray Timing Explorer}}）的正比计数器阵列（PCA）对吸积动力X射线脉冲星Cen X-3的准周期振荡（QPO）特征进行了为期4年的观测。观测涵盖了宽范围的X射线强度的源超过二进制强度调制。我们已经检测到QPO在11个共81点的PCA与均方根强度波动高达10%。QPO峰值频率在40和90 mHz附近显示出聚类，QPO频率与X射线强度无关。这表明，要么（a）观测到的X射线亮度的源是不相关的质量吸积率或吸积盘的内半径或（b）QPO的产生机制在岑X-3是不同的拍频模型或开普勒频率模型，被认为是在大多数其他瞬态和持久的X射线天体运行。我们还发现，在40 mHz的QPO特征的均方根变化是不依赖于X射线的能量，这表明盘吸收有关的起源QPO是不可能的。
英文摘要：
We have investigated properties of the Quasi Periodic Oscillation (QPO) features in the accretion powered X-ray pulsar Cen X-3 over a period of about four years using observations carried out with the Proportional Counter Array (PCA) of the {\it {Rossi X-ray Timing Explorer}}. The observations cover a wide range of X-ray intensity of the source in excess of the binary intensity modulation. We have detected QPOs in 11 out of a total 81 pointings with the PCA with rms intensity fluctuation upto 10%. The QPO peak frequency shows clustering around 40 and 90 mHz with the QPO frequency having no dependence on X-ray intensity. This indicates that either (a) the observed X-ray luminosity of the source is not related to the mass accretion rate or inner radius of the accretion disk or (b) that the QPO generation mechanism in Cen X-3 is different from the beat frequency model or Keplerian frequency model that is believed to be operational in most other transient and persistent X-ray pulsars. We have also found that, the rms variation in the 40 mHz QPO feature is not dependent on the X-ray energy, indicating that disk absorption related origin for the QPO is unlikely.
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