从GX 339-4的X射线和光学光变曲线中提取共同信号成分：反相关的新观点
Extracting common signal components from the X-ray and optical light curves of GX 339-4: new view for anti-correlation
摘要：
对黑洞X射线双星的同时X射线和光学观测表明，当天体处于硬态时，其光变曲线包含多个相关和反相关的变化分量。在黑洞X射线双星GX 339-4的情况下，光变曲线的互相关联函数（CCF）表明与0.15 s的光学滞后正相关，与1 s的光学滞后和4 s的X射线滞后反相关。这表明两个光变曲线具有一些具有不同延迟的共同信号分量。在这项研究中，我们从GX 339-4的数据中提取并重建了这些信号分量。结果证实了相关和反相关与光学滞后是两个共同的组成部分。然而，我们发现，重建的光变曲线的反相关组件表示一个正相关的变化与X射线滞后~ +1秒。此外，该信号分量的CCF不仅与光学滞后，而且与X射线滞后显示出反相关性，这与数据的CCF一致。因此，我们的研究结果表明，两个正相关分量的组合，即具有0.15-s光学滞后的X射线先行信号和具有1-s X射线滞后的光学先行信号，可以使观察到的CCF没有反相关信号。光学先行信号可能是由磁吸积流或喷流中的同步辐射引起的，而X射线时间滞后的机制还需要进一步研究。
英文摘要：
Simultaneous X-ray and optical observations of black hole X-ray binaries have shown that the light curves contain multiple correlated and anti-correlated variation components when the objects are in the hard state. In the case of the black hole X-ray binary, GX 339-4, the cross correlation function (CCF) of the light curves suggests a positive correlation with an optical lag of 0.15 s and anti-correlations with an optical lag of 1 s and X-ray lag of 4 s. This indicates the two light curves have some common signal components with different delays. In this study, we extracted and reconstructed those signal components from the data for GX 339-4. The results confirmed that correlation and anti-correlation with the optical lag are two common components. However, we found that the reconstructed light curve for the anti-correlated component indicates a positively correlated variation with an X-ray lag of ~ +1 s. In addition, the CCF for this signal component shows anti-correlations not only with the optical lag, but also with the X-ray lag, which is consistent with the CCF for the data. Therefore, our results suggest that the combination of the two positively correlated components, that is, the X-ray preceding signal with the 0.15-s optical lag and the optical preceding signal with the 1-s X-ray lag, can make the observed CCF without anti-correlated signals. The optical preceding signal may be caused by synchrotron emission in a magnetically dominated accretion flow or in a jet, while further study is required to understand the mechanism of the X-ray time lag.
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