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

1996年，首席研究员大阪洋次在圆盘不稳定性模型的基本框架内提出了一个矮新星爆发的统一模型。我的研究基本上是沿着这条线进行的延续。现将我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星的重复再亮现象。(2)提出了WZ SGE星爆发早期观测到的“早期驼峰”现象是极低质量比双星系统吸积盘潮汐2：1共振的表现。(3)我们仔细研究了次级恒星爆发期间质量传递增强的观测证据，并证明大多数质量传递增强的证据并不充分。(4)提出了WZSGE 2001年突出复杂超峰光曲线分析的新方法。这种方法被称为吸积盘的螺旋层析成像，因为它可以重建不同超峰时期的一系列盘图像。

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.