Mass-transfer in close binary and their companions

Wenping Liao, Shengbang Qian, Liying Zhu & Linjia Li

Yunnan Observatories, Chinese Academy of Sciences

Secular and/or cyclical orbital period variations of close binaries can be derived by analyzing the (O-C) diagram. The secular variations are usually explained as mass transfer between components, while the most plausible explanation of the cyclic period changes is the LTTE through the presence of a third body. Mass transfer and additional components in close binary systems are important for understanding the formation and evolution of close binary stars. In this paper, some new results of photometric analysis of several close binaries are present.

Last update: