Photometric monitoring of the ROSAT selected late type stars |
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| Institution: | 1. Department of Technology and Physics, Zhengzhou University of Light Industry, Zhengzhou 450002, China;2. National Astronomical Observatories, Chinese Academy of Sciences, Beijing 100012, China;1. Department of Mathematics, The University of Hong Kong, Pokfulam Road, Hong Kong, People''s Republic of China;2. ACSys CRC, CSIRO Mathematical and Information Sciences, GPO Box 664, Canberra, ACT 2601, Australia;1. Department of Geology and Planetary Science, University of Pittsburgh, Pittsburgh, Pennsylvania, 15260;2. Jet Propulsion Laboratory, Pasadena, California, 91109;1. Department of Chemistry, Iowa State University, Ames, IA 50011, USA;2. Department of Biomedical Engineering, State University of New York at Stony Brook, NY 11794-2580, USA;3. Department of Chemistry, Wuhan University, Wuhan 430072, People''s Republic of China;1. Dipartimento di Ingegneria dell’Innovazione, Università di Lecce and INFN Sezione di Lecce, Via Monteroni, 73100 Lecce, Italy;2. Joint Center for Earth Systems Technology (JCET/UMBC), University of Maryland, Baltimore County, 1000 Hilltop Circle, Baltimore, MD 21250, USA;3. Dipartimento di Fisica, Università di Lecce and INFN Sezione di Lecce, Via Arnesano, 73100 Lecce, Italy |
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| Abstract: | We monitored the light variations of 16 solar-type stars recently discovered in the X-ray wave-length range during the ROSAT all-sky survey. We find that 9 out of 16 stars showed appreciable light variability with amplitudes of a few hundredths of a magnitude. They are all proved to be in periodic variations. Using the methods of the phase dispersion minimization (PDM) and Fourier Analysis (PERIOD04), we derive the photometric periods for these stars. The rotational periods are found range from 0.471 to 17.31 days and the period of stars most (of 7 stars) being shorter than 3 days. Apart from binaries system, the results give further evidence for the spin up of solar-type stars as predicted by models of angular momentum evolution of pre-main sequence stars. |
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