| Rotation Periods of Nine ROSAT Selected Solar-Type Stars |
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| 作者姓名： | Li-Feng Xing Shuang-Yi Zhao Wei Su Yan Shen Xiao-Bin Zhang Jian-Yan Wei |
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| 作者单位： | Li-Feng Xing1，2，Shuang-Yi Zhao3，Wei Su2，Yan Shen1，Xiao-Bin Zhang2 and Jian-Yan Wei2 1 Department of Technology and Physics，Zhengzhou University of Light Industry，Zhengzhou 450002; 2 National Astronomical Observatories，Chinese Academy of Sciences，Beijing 100012 3 Department of Physics，Xingtai University，Xingtai 054001 |
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| 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 3days. 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.
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| 关 键 词： | stars: late-type — stars: pre-main sequence — stars: rotation |
| 修稿时间： | 2006-08-03 |
Rotation Periods of Nine ROSAT Selected Solar-Type Stars |
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| Li-Feng Xing Shuang-Yi Zhao Wei Su Yan Shen Xiao-Bin Zhang Jian-Yan Wei.Rotation Periods of Nine ROSAT Selected Solar-Type Stars[J].Chinese Journal of Astronomy and Astrophysics,2007,7(4):551-557. |
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| Authors: | Li-Feng Xing Shuang-Yi Zhao Wei Su Yan Shen Xiao-Bin Zhang Jian-Yan Wei |
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| Abstract: | 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 3days. 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. |
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| Keywords: | stars: late-type - stars: pre-main sequence - stars: rotation |
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