微类星体SS433吸积盘的流入和流出：UKIRT光谱学
Inflow and outflow from the accretion disc of the microquasar SS433: UKIRT spectroscopy
摘要：
在SS 433轨道的整个周期中每晚进行的一系列近红外光谱观测揭示了：（i）SS 433吸积盘的持续特征，其旋转速度约为500 km/s，（ii）布伦德尔最近在光学波长处发现的环双星盘的存在，Bowler和Schmidtobreick（2008）和（iii）比以前测量的盘风更快的外流。从这些，我们发现一个更快的吸积盘风比以前注意到的，终极速度~1500公里/秒。风终极速度的增加导致质量损失率约为10 e-4 M_sun/yr。这些数据与新确定的SS 433系统部件的质量（向上）一起，可准确诊断SS 433具有超爱丁顿流的程度。我们的观测结果表明伴星的大小与轨道的半短轴相当，轨道的半短轴由（1-e^2）^（1/2）40 R_sun给出，其中e是离心率。我们在这些近红外波长的相对较高的光谱分辨率使我们能够解构组成这个二元系统中的Brackett-gamma线的不同成分及其物理起源。由于这条线在我们的一系列观测中占主导地位的盘风，吸积盘本身只有少数（~ 15%）的贡献，我们警告不要使用未解决的Brackett-gamma线强度作为“吸积签名”在X射线双星或微类星体以任何定量的方式。
英文摘要：
A succession of near-IR spectroscopic observations, taken nightly throughout an entire cycle of SS433's orbit, reveal (i) the persistent signature of SS433's accretion disc, having a rotation speed of ~500 km/s, (ii) the presence of the circumbinary disc recently discovered at optical wavelengths by Blundell, Bowler and Schmidtobreick (2008) and (iii) a much faster outflow than has previously been measured for the disc wind. From these, we find a much faster accretion disc wind than has noted before, with a terminal velocity of ~1500 km/s. The increased wind terminal velocity results in a mass-loss rate of ~10e-4 M_sun/yr. These, together with the newly (upwardly) determined masses for the components of the SS433 system, result in an accurate diagnosis of the extent to which SS433 has super-Eddington flows. Our observations imply that the size of the companion star is comparable with the semi-minor axis of the orbit which is given by (1-e^2)^(1/2) 40 R_sun, where e is the eccentricity. Our relatively high spectral resolution at these near-IR wavelengths has enabled us to deconstruct the different components that comprise the Brackett-gamma line in this binary system, and their physical origins. With this line dominated throughout our series of observations by the disc wind, and the accretion disc itself being only a minority (~15 per cent) contribution, we caution against use of the unresolved Brackett-gamma line intensity as an "accretion signature" in X-ray binaries or microquasars in any quantitative way.
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