Research on Outburst Mechanisms of Dwarf Novae and Evolution of Cataclysmic Variable Stars

1996年，首席研究员Yoji Osaki在磁盘不稳定性模型的基本框架内提出了矮新星爆发的统一模型。我的研究基本上是沿着这条路线的延续。我在2002-2003年的研究成果总结如下：(1)我们提出了一个新的模型来解释WZ Sge恒星的重复再亮。(2)提出WZ - Sge恒星爆发初期观测到的“早驼峰”现象是极低质量比双星系统吸积盘中潮汐型2:1共振的表现。(3)我们严格审查了在爆发期间从副恒星增强传质的观测证据，并证明大多数增强传质的证据并没有得到很好的证实。(4)提出了分析2001年WZ Sge爆发的复杂超峰光曲线的新方法。这种方法被称为吸积盘的螺旋层析成像，因为它可以在不同的超级峰期重建一系列的磁盘图像。

Yoji Osaki, the head investigator, proposed a unification model for dwarf nova outbursts within the basic framework of the disk instability model in 1996. My research is basically a continuation along this line. My research results in 2002-2003 are summarized below. (1) We have proposed a new model to explain repetitive rebrightemng in WZ Sge stars. (2) We have proposed that the "early hump" phenomenon observed in the early phase of outbursts of WZ Sge stars is, the manifestation of the tidal 2:1 resonance in accretion disks of binary systems with extremely low mass ratios. (3) We have critically examined observational evidence for enhanced mass transfer from the secondary star during outbursts and demonstrated that most evidence for enhanced mass transfer is not well substantiated. (4) I have proposed a new method for analyzing complex superhump light curves for the 2001 outburst of WZ Sge. This method is called a helical tomography of an accretion disk because it can reconstruct a series of disk images at different superhump period.