Optically Thick Wind Theory and its application to Binary Evolution Associate Prof.

1.新星的光曲线分析利用光学厚风理论建立了经典新星的光曲线分析。这是一种测定双星白矮星质量的新方法。Ia型超新星的先驱光厚的风控制着双星演化，因为风带走了系统的角动量和质量。我们将这种风效应纳入双星演化中，发现了超软X射线通道和共生通道两种新的Ia超新星前身分类方法。重现新星与Ia型超新星的关系通过对9颗重现新星的光曲线分析，发现大部分重现新星都处于Ia型超新星爆发前的阶段。极大质量主序列的结构由于不透明度中的铁峰，即使在主序列阶段，极大质量恒星也具有核-晕结构。光球层温度随着恒星质量的增加而降低，这与观测特性是一致的。

The main results of this research is summarized as follows :1. Light curve analysis of novaeI established light curve analysis of classical nova using optically thick wind theory. This is a new method to determine the white dwarf mass of binaries.2. Progenitor of Type Ia SupernovaeThe optically thick wind governs the binary evolution, because the wind carries away the angular momentum and the mass from the system. We include this effects of the wind into the binary evolution and found two new ways to type Ia supernova progenitor : Super-soft X-ray channel and the Symbiotic channel.3. Relation between Recurrent Novae and Type Ia SupernovaDetailed light curve analysis of nine recurrent novae, we find that most of the recurrent nova is in the stage just before the type Ia supernova explosion.4. Structure of Very Massive Main-SequenceVery massive stars have a core-halo structure even in the main-sequence stage due to the iron peak in the opacity. The photospheric temperature decreases as the stellar mass increases, which is consistent with observational properties.