| 其他摘要 | Binary systems make up about half of all celestial systems, and close binary systems generate many special astronomical phenomena through material exchange or gravitational interactions, such as type Ia supernovae, supersoft X-ray sources, cataclysmic variables, and fast radio bursts. These special astronomical phenomena are important tools for studying stellar and even cosmic evolution. In some interacting binary systems, such as supersoft X-ray sources, have high radiation luminosity in the supersoft X-ray band. When the intense radiation irradiates the companion star, it heats up the companion star and causes changes, such as an increased transfer rate due to expansion and increased luminosity. In the work, we mainly study irradiation-driven mass transfer and feedback from the companion star in binary systems, summarized as follows:The research had four main areas of study. First, we explored the origin of quasi-periodic optical light curves in supersoft X-ray sources. We hypothesized that periodic variations in supersoft X-rays could lead to a periodic variation in mass transfer rate. We gave the white dwarf a periodically accretion rate, and the white dwarf periodically expanded and contracted under such an accretion rate, thus reproducing the quasi-periodic light curve of supersoft X-ray sources.Second, we studied the feedback of the companion star to the irradiation of supersoft X-rays. We found that under periodic X-ray irradiation and heating by supersoft X-rays, the companion star expands or constant, and then the mass transfer rate also shows periodic increases or decreases. These changes in mass transfer rate can essentially reproduce the periodic-shaped accretion rate used in the above work. Based on these results, we concluded that the mechanism of supersoft X-ray irradiation on the companion star is the origin of the quasi-periodic variation in the optical light curve of supersoft X-ray sources.Third, we investigated the effects of nova eruptions on binary systems. We found that the surface of the companion star expands, and the mass transfer rate increases due to the irradiation of the nova eruption luminosity and white dwarf accretion luminosity. If the mass transfer rate stabilizes and continues for thousands of years, the nova system will transform into a supersoft X-ray source system. We calculated the parameter space of white dwarf and companion star mass for nova systems to become supersoft X-ray source systems after the eruption.In the future work, we will calculate the increased birth rate of Type Ia supernovae accordingly.Finally, we studied the effects of fast radio bursts (FRBs) on binary systems. We focused on systems composed of a neutron star and a low-mass main-sequence companion, assuming that the FRB comes from the neutron star. We found that the large radio energy of FRBs may heat up the companion star, causing the companion star to exhibit re-emission features. This re-emission feature may be detected in multi-band observations of fast radio bursts in the Milky Way, which will help us understand the physical mechanisms and origins of fast radio bursts. |
修改评论