食HMXB 4 U 1700-37的轨道演化和偏心率及拱点运动的研究
Orbital evolution and search for eccentricity and apsidal motion in the eclipsing HMXB 4U 1700-37
摘要：
在食X射线双星4U 1700-37中没有可探测到的脉动的情况下，轨道周期衰减必须从食定时测量中确定。我们使用了早期报道的4U 1700-37的日食中期时间测量结果，以及全天空监视器RXTE-ASM，Swift-BAT和MAXI-GSC获得的长期光变曲线的新测量结果，以及RXTE-PCA的观测结果，来测量双星的长期轨道演化。该系统的轨道周期衰减率估计为${\dot{P}}/P = -(4.7 \pm 1.9) \times 10^{-7}$ yr $^{-1}$，小于以前的估计。我们还使用了从10年长的X射线光变曲线与Swift-BAT获得的日食中期时间和日食持续时间的测量，分别对双星系统的偏心率施加约束，并试图测量任何拱点运动。当拱点运动速率大于每年5度时，偏心率小于0.008，这限制了我们从现有数据确定拱点运动速率的能力。我们讨论了目前的偏心率极限与早期报道的伴星径向速度测量值的差异。
英文摘要：
In the absence of detectable pulsations in the eclipsing High Mass X-ray binary 4U 1700-37, the orbital period decay is necessarily determined from the eclipse timing measurements. We have used the earlier reported mid-eclipse time measurements of 4U 1700-37 together with the new measurements from long term light curves obtained with the all sky monitors RXTE-ASM, Swift-BAT and MAXI-GSC, as well as observations with RXTE-PCA, to measure the long term orbital evolution of the binary. The orbital period decay rate of the system is estimated to be ${\dot{P}}/P = -(4.7 \pm 1.9) \times 10^{-7}$ yr$^{-1}$, smaller compared to its previous estimates. We have also used the mid-eclipse times and the eclipse duration measurements obtained from 10 years long X-ray light-curve with Swift-BAT to separately put constraints on the eccentricity of the binary system and attempted to measure any apsidal motion. For an apsidal motion rate greater than 5 degrees per year, the eccentricity is found to be less than 0.008, which limits our ability to determine the apsidal motion rate from the current data. We discuss the discrepancy of the current limit of eccentricity with the earlier reported values from radial velocity measurements of the companion star.
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