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arXiv 0810.0432astro-ph
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用XMM-Newton和INTEGRAL观测的低质量X射线双星XB 1254-69倾角特性的变化

Variations in the dip properties of the low-mass X-ray binary XB 1254-69 observed with XMM-Newton and INTEGRAL

M. Diaz Trigo, A. N. Parmar, L. Boirin, C. Motch, A. Talavera, S. Balman

备注：
16 pages, 10 figures, 4 tables. Accepted for publication in A&A
发表信息：
PoS MQW7:058,2008
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摘要：

我们分析了XB 1254-69的五个XMM-牛顿观测数据，其中一个与INTEGRAL同时进行，以研究从这个低质量X射线双星中看到的高度可变的倾角持续时间和深度的机制。在两次观测中出现了深倾斜，在一次观测中出现了浅倾斜，在其余两次观测中没有检测到倾斜。在高（1-4秒）时间分辨率下，可以看到“浅倾角”包括一些非常快速的深倾角，而“深”倾角由许多类似的非常快速的深波动组成。折叠V波段光学监测器光变曲线在光源经历深、浅和不可检测的倾斜时表现出不同幅度和相位的正弦变化。我们适合EPIC光谱获得的“持久性”或无倾角的间隔与一个模型组成的磁盘黑体和热comptonisation组件与高斯发射功能在1和6.6千电子伏修改吸收由于冷和光电离材料。没有一个光谱参数似乎与倾角深度有很强的相关性，除了盘黑体的温度，当存在深倾角时，盘黑体的温度最冷（kT ~ 1.8 keV），当没有倾角时，盘黑体的温度最热（kT ~ 2.1 keV）。我们建议，在光盘温度和光学调制的变化可以解释的存在下，在系统中的倾斜吸积盘。我们提供了一个修正后的轨道周期估计为0.16388875 +/- 0.00000017天。

英文摘要：

We have analysed data from five XMM-Newton observations of XB 1254-69, one of them simultaneous with INTEGRAL, to investigate the mechanism responsible for the highly variable dips durations and depths seen from this low-mass X-ray binary. Deep dips were present during two observations, shallow dips during one and no dips were detected during the remaining two observations. At high (1-4 s) time resolution ``shallow dips'' are seen to include a few, very rapid, deep dips whilst the ``deep'' dips consist of many similar very rapid, deep, fluctuations. The folded V-band Optical Monitor light curves obtained when the source was undergoing deep, shallow and no detectable dipping exhibit sinusoid-like variations with different amplitudes and phases. We fit EPIC spectra obtained from "persistent" or dip-free intervals with a model consisting of disc-blackbody and thermal comptonisation components together with Gaussian emission features at 1 and 6.6 keV modified by absorption due to cold and photo-ionised material. None of the spectral parameters appears to be strongly correlated with the dip depth except for the temperature of the disc blackbody which is coolest (kT ~ 1.8 keV) when deep dips are present and warmest (kT ~ 2.1 keV) when no dips are detectable. We propose that the changes in both disc temperature and optical modulation could be explained by the presence of a tilted accretion disc in the system. We provide a revised estimate of the orbital period of 0.16388875 +/- 0.00000017 day.

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