最近一些年，随着太空观测项目CoRoT和Kepler的开展，观测到一批g模式脉动特征的B型亚矮（sdB）星。这些脉动sdB星的周期间隔均被精确的测量出来，分布在230至275s之间。sdB星中心对流核的大小具有极大的不确定性，这取决于其边界处的超射处理方式。目前的已知的超射处理方式包括标准的对流超射、半对流、最大化对流超射和κ-ω模型。不同的超射处理会使中心对流核大小的增长情况不一样，对周期间隔的影响也不一样。本项目将在模型中分别考虑四种超射处理对周期间隔的影响，再与观测数据进行比较，从而找出最为合理的超射模型。最后，利用最为合理的超射模型分析周期间隔对对流核大小的限制情况。这项研究对检验对流超射理论和探索sdB星中心对流核的大小有着重要的科学价值。

Recently, some g-mode pulsating subdwarf B (sdB) stars have been detected with the advent of the space missions CoRoT and Kepler. The period spacings of these pulsating sdB stars are accurately measured, ranging from 230 to 275s. The size of the convective core in the center of sdB stars are quite uncertain, which depend on the method of overshoot at their boundaries. At present, the known methods of overshoot include standard overshoot, semiconvection, maximal overshoot and the κ-ω model. Different method of overshoot will make the size of central convective core grow differently and affect the period spacings differently. In this project, the influence of four kinds of overshoot on the period spacings will be considered in the models, and then the most reasonable overshooting model will be found by comparing with the observations. Finally, the most reasonable overshooting model is used to analyze the limitation of the period spacings on the size of convective core. This project has important scientific values for testing the theories of convective overshoot and exploring the size of central convective core in sdB stars.