Eclipse Mapping of Accretion Disks: The First Decade
Eclipse Mapping of Accretion Disks: The First Decade
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吸积盘的日食测绘：第一个十年
DOI：
10.1142/9789814350976_0005
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发表时间：
1993
期刊：
影响因子：
--
通讯作者：
K. Horne
中科院分区：
文献类型：
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作者：
K. Horne
日食光曲线的观测正在被用来绘制食突变变星中的吸积盘的地图。通过观察真实吸积盘的结构，我们可以检验吸积盘大气结构的模型，通过跟踪经历爆发的矮新星盘结构的时间变化来了解吸积盘的粘性，并测量系统中不同双星周期的质量吸积率，以检验关于激变变星长期演化的想法。在爆发期间和长周期类新星变星中观测到的矮新星的盘结构证实了理论预测的定态盘的TαR-3/4定律。然而，在静止的矮新星的圆盘中发现了更平坦的径向轮廓，它们看起来很薄，而且在周期在3到4小时之间的新星变星中发现了更平坦的径向轮廓，这可能是驱动吸积盘风的原因。本章回顾了日食映射方法，并讨论了吸积盘映射对吸积盘理论提出的一些挑战。
Observations of eclipse light curves are being used to make maps of the accretion disks in eclipsing cataclysmic variables. By observing the structure of real accretion disks, we can test models of the structure of accretion disk atmospheres, learn about accretion disk viscosity by tracking time-variations in the structure of dwarf nova disks undergoing outbursts, and measure mass accretion rates in systems at different binary periods to test ideas about the long-term evolution of cataclysmic variables. The observed disk structures in dwarf novae during outburst and in long-period nova-like variables confirm the T α R-3/4law predicted by theory for steady-state disks. However, much flatter radial profiles are found in the disks of quiescent dwarf novae, which appear to be optically-thin, and in nova-like variables with periods between 3 and 4 hours, which may be driving an accretion disk wind. This chapter reviews eclipse mapping methods, and discusses some of the challenges that accretion disk maps are presenting to accretion disk theory.