Maximum Entropy Reconstruction of Accretion Disk Images from Eclipse Data
Maximum Entropy Reconstruction of Accretion Disk Images from Eclipse Data
复制标题
根据日食数据对吸积盘图像进行最大熵重建
DOI：
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发表时间：
1985
期刊：
影响因子：
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通讯作者：
K. Horne
中科院分区：
文献类型：
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作者：
K. Horne
食灾变变星为吸积盘理论的观测检验提供了一个独特的机会。激变变星是由一颗吸积的白色矮星和一颗充满其罗奇叶的晚型次级星星组成的近距离双星系统。白色矮星周围的吸积盘是由一股气体流供给的，该气体流是从靠近内拉格朗日点的次级星星中产生的。一个紧凑的明亮的区域经常出现在流注入新鲜的物质到吸积盘。在大多数情况下，星盘是系统中的主要光源，次级星星的光度相对较小。因此，次级星星的引力就像是吸积流空间结构的精确探测器。
The eclipsing cataclysmic variables provide a unique opportunity for the observational testing of accretion disk theory. Cataclysmic variables (CVs) are close binary systems which consist of an accreting white dwarf primary, and a late-type secondary star that fills its Roche-lobe. The accretion disk around the white dwarf is fed by a gas stream which emerges from the secondary star near the inner Lagrangian point. A compact bright region is frequently present where the stream injects fresh material into the accretion disk. In most cases the disk is the dominant source of light in the system, and the luminosity of the secondary star is comparatively small. Eclipses by the secondary star thus act as precise probes of the spatial structure of the accretion flow.