从衰减盘风看SS433的环双星环和吸积盘
SS433's circumbinary ring and accretion disc viewed through its attenuating disc wind
摘要：
我们目前的光谱学的微类星体SS 433涵盖了一个重要的部分，其喷流轴的岁差周期。主要的稳定H-α和H-β谱线的分量主要被确定为来自三个发射区域：（i）一个超级爱丁顿吸积盘风，以一个广泛的组成部分的形式占大部分的质量损失从系统，（ii）一个环双星盘的材料，我们假设是通过双星的L2点排泄，以及（iii）吸积盘本身作为两个显着持久的成分。吸积盘的组成部分在盘的外部区域以~600 km/s的开普勒速度移动。这种分解的直接结果是确定了吸积盘的大小，在围绕质量为10 M_sun的黑洞的开普勒轨道情况下，吸积盘的外半径达到~8 R_sun。我们确定了SS 433中吸积盘内外半径比的一个上限，R_in/R_out ~ 0.2，与致密天体的质量无关。巴耳末减量，H-α/H-β，从适当的固定发射线为系统的每个组件提取。导出了气体组分的物理参数。环双星环的衰减量在整个岁差阶段似乎是相当恒定的，这意味着环双星盘的电子密度为log N_e（cm^-3）~ 11.5。吸积盘风的衰减变化较大，表现出明显的岁差相位依赖性，这意味着在10 ~ 13之间，吸积盘风的电子密度log N_e（cm^-3）沿我们的视线呈正弦变化。这种密度与方向的依赖性表明吸积盘风的性质是类旋波的。
英文摘要：
We present optical spectroscopy of the microquasar SS433 covering a significant fraction of a precessional cycle of its jet axis. The components of the prominent stationary H-alpha and H-beta lines are mainly identified as arising from three emitting regions: (i) a super-Eddington accretion disc wind, in the form of a broad component accounting for most of the mass loss from the system, (ii) a circumbinary disc of material that we presume is being excreted through the binary's L2 point, and (iii) the accretion disc itself as two remarkably persistent components. The accretion disc components move with a Keplerian velocity of ~600 km/s in the outer region of the disc. A direct result of this decomposition is the determination of the accretion disc size, whose outer radius attains ~8 R_sun in the case of Keplerian orbits around a black hole mass of 10 M_sun. We determine an upper limit for the accretion disc inner to outer radius ratio in SS433, R_in/R_out ~ 0.2, independent of the mass of the compact object. The Balmer decrements, H-alpha/H-beta, are extracted from the appropriate stationary emission lines for each component of the system. The physical parameters of the gaseous components are derived. The circumbinary ring decrement seems to be quite constant throughout precessional phase, implying a constant electron density of log N_e(cm^-3) ~ 11.5 for the circumbinary disc. The accretion disc wind shows a larger change in its decrements exhibiting a clear dependence on precessional phase, implying a sinusoid variation in its electron density log N_e(cm^-3) along our line-of-sight between 10 and 13. This dependence of density on direction suggests that the accretion disc wind is polloidal in nature.
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