黑洞双星A0620-00的多普勒层析成像和静止X射线双星色球发射的起源
Doppler tomography of the black hole binary A0620-00 and the origin of chromospheric emission in quiescent X-ray binaries
摘要：
在低质量X射线双星的发射线轮廓的多普勒层析成像，使我们能够解开不同的发射网站和研究的结构和变化的吸积盘。本文报道了黑洞双星A0620-00在静止状态下的UVES高分辨率光谱观测结果，这些光谱数据约束了轨道参数Porb=0.32301405（1）d和K ~ 2 =437.1 ± 2.0 km/s。这些值，加上质量比q=M2/M1=0.062+-0.010，意味着致密天体的最小质量为M1（sin i）^3=3.15+-0.10 Msun，这与以前的工作是一致的。来自吸积盘的H $α$发射比以前的研究弱得多，这可能是由于吸积盘活动的减少。H $α$谱线的多普勒成像首次显示了一个来自第二颗恒星的窄分量，观测到的等效宽度为1.4 ± 0.3埃，可能与色球活动有关。减去一颗K型模板星，并对吸积盘的遮蔽进行修正，得到的等效宽度为2.8 ± 0.3埃。在气流轨迹与吸积盘相交的位置上也探测到一个亮的热点。与第二颗星相关的H $α$通量太大，无法通过X射线照射提供动力。它与具有类似轨道周期的RS CVn双星中观察到的情况相当，因此可能是由快速的恒星旋转引发的。
英文摘要：
Doppler tomography of emission line profiles in low mass X-ray binaries allows us to disentangle the different emission sites and study the structure and variability of accretion disks. We present UVES high-resolution spectroscopic observations of the black hole binary A0620-00 at quiescence.These spectroscopic data constrain the orbital parameters Porb=0.32301405(1) d and K2=437.1+-2.0 km/s. These values, together with the mass ratio q=M2/M1=0.062+-0.010, imply a minimum mass for the compact object of M1(sin i)^3=3.15+-0.10 Msun, consistent with previous works.The H$α$ emission from the accretion disk is much weaker than in previous studies, possibly due to a decrease in disk activity. Doppler imaging of the H$α$ line shows for the first time a narrow component coming from the secondary star, with an observed equivalent width of 1.4+-0.3 Angstroms, perhaps associated to chromospheric activity. Subtracting a K-type template star and correcting for the veiling of the accretion disk yields to an equivalent width of 2.8+-0.3 Angstroms. A bright hot-spot is also detected at the position where the gas stream trajectory intercepts with the accretion disk. The H$α$ flux associated to the secondary star is too large to be powered by X-ray irradiation. It is comparable to those observed in RS CVn binaries with similar orbital periods and, therefore, is probably triggered by the rapid stellar rotation.
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