In X-ray binaries, rapid variability in X-ray flux of greater than an order of magnitude on time-scales of a day or less appears to be a signature of wind accretion from a supergiant companion. When the variability takes the form of rare, brief, bright outbursts with only faint emission between them, the systems are called Supergiant Fast X-ray Transients (SFXTs). We present data from twice-weekly scans of the Galactic bulge by the Rossi X-ray Timing Explorer (RXTE) that allow us to compare the behaviour of known SFXTs and possible SFXT candidates with the persistently bright supergiant X-ray binary 4U 1700-377. We independently confirm the orbital periods reported by other groups for SFXTs SAX J1818.6-1703 and IGR J17544-2619. The new data do not independently reproduce the orbital period reported for XTE J1739-302, but slightly improve the significance of the original result when the data are combined. The bulge source XTE J1743-363 shows a combination of fast variability and a long-term decline in activity, the latter behaviour not being characteristic of supergiant X-ray binaries. A far-red spectrum of the companion suggests that it is a symbiotic neutron star binary rather than a high-mass binary, and the reddest known of this class: the spectral type is approximately M8 III.
Temporal and spectral evolution in X- and gamma-rays of magnetar 1E 1547.0-5408 since its October 2008 outburst: the discovery of a transient hard pulsed component after its January 2009 outburst
磁星1 E 1547.0-5408在2008年10月和2009年1月爆发。在本文中，我们详细介绍了从2008年10月3日开始到2011年1月结束的1 E 1547.0-5408在~1和300 keV之间持续总发射和脉冲发射的时间和光谱特征的演变。我们分析了罗西X射线计时探测器，国际伽马射线天体物理实验室和斯威夫特卫星收集的数据。
Studies of the Origin of High-Frequency Quasi-Periodic Oscillations of Mass Accreting Black Holes in X-ray Binaries with Next-Generation X-ray Telescopes
Variability in the orbital profiles of the X-ray emission of the gamma-ray binary LS I +61 303
利用Rossi X射线定时探测器（RXTE）正比计数器阵列（PCA）对$γ$双星LS I +61 303进行了35个完整的轨道运动周期的观测分析。这构成了迄今为止针对该来源分析的最大连续X射线监测数据集。这种扩展分析使我们能够报告：a）发现X射线发射的轨道轮廓的可变性，b）在源的典型总体行为之上存在几个（最近的）短耀斑，给定PCA视场，其可能与或可能不与LS I +61 303相关联，和c）仅使用软X射线数据确定轨道周期。
