Rotation Periods of Nine ROSAT Selected Solar-Type Stars

作     者：Li-Feng Xing Shuang-Yi Zhao Wei Su Yan Shen Xiao-Bin Zhang Jian-Yan Wei 

作者机构：Department of Technology and Physics Zhengzhou Unversity of Light Industry Zhengzhou 450002 National Astronomical Observatories Chinese Academy of Sciences Beijing 100012 Department of Physics Xingtai University Xingtai 054001 

出 版 物：《Chinese Journal of Astronomy and Astrophysics》 (中国天文和天体物理学报（英文版）)

年 卷 期：2007年第7卷第4期

页      面：551-557页

核心收录：

学科分类：07[理学] 070401[理学-天体物理] 0704[理学-天文学] 

基　　金：the National Natural Science Foundation of China 

主　　题：stars: late type   stars: pre main sequence   stars: rotation 

摘      要：We monitored 16 X-ray selected young solar-type stars for light variation and found appreciable periodic light variability with amplitudes of a few hundredths of a magni- tude in nine of the objects. Using the method of Phase Dispersion Minimization （PDM） and Fourier analysis （software PERIOD04）, the rotation periods of these stars were determined from the photometric data. The rotation periods of all nine stars are shorter than about 3 days. It is suggested that, as with the Pleiades cluster, small amplitude light variations are quite common among young solar-type stars with rotation periods around 3 days or less. This gives further evidence for the spin up of solar-type stars predicted by models of angular momentum evolution of pre-main sequence stars.