Is the β Pictoris member GJ 3039AB a physical binary? What the rotation periods tell us? |
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| Institution: | 1. INAF- Catania Astrophysical Observatory, via S.Sofia, 78 I-95123 Catania, Italy;2. Montcabrer Observatory, C/Jaume Balmes, 24, Cabrils, Spain;3. Aryabhatta Research Institute of Observational Sciences, Manora Peak, Nainital 263129, India;1. College of Science/Department of Physics & NAOC-GZU-Sponsored Center for Astronomy Research, Guizhou University, Guiyang 550025, P.R. China;2. Key Laboratory for the Structure and Evolution of Celestial Objects, Chinese Academy of Sciences, Kunming 650011, P.R. China;3. Dept. of Physics and Astronomy, Butler University, Indianapolis, IN 46208, USA;4. National Astronomical Observatories/Yunnan Observatory, Chinese Academy of Sciences, Kunming, 65 0011, P.R. China;1. College of Science/Department of Physics & NAOC-GZU-Sponsored Center for Astronomy Research, Guizhou University, Guiyang 550025, PR China;2. Key Laboratory for the Structure and Evolution of Celestial Objects, Chinese Academy of Sciences, Kunming 650011, PR China;3. Department of Physics and Astronomy, Butler University, Indianapolis, IN 46208, USA;1. Institute of Astronomy and National Astronomical Observatory, Bulgarian Academy of Sciences, 72 Tsarigradsko Shose blvd., 1784 Sofia, Bulgaria;2. Armagh Observatory, College Hill, Armagh BT619DG, Northern Ireland, UK;1. School of Information Science and Engineering, University of Jinan, Shandong Provincial Key Laboratory of Network Based Intelligent Computing, Jinan 250022, China;2. China Academy of Science, Key Laboratory of Solar Activity, Peking 100012, China;1. Physics Research Centre, VHNSN College, Virudhunagar – 626 001, India;2. Physics Research Centre, NMSSVN College, Madurai – 625 019, India;3. Madurai Kamaraj University Constituent College, Thirumangalam – 625 706, India |
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| Abstract: | We have carried out a multi-band photometric monitoring of the close visual binary GJ 3039, consisting of a M4 primary and a fainter secondary component, and likely member of the young stellar association β Pictoris (24-Myr old). From our analysis we found that both components are photometric variables and, for the first time, we detected two micro-flare events. We measured from periodogram analysis of the photometric time series two rotation periods P = 3.355 d and P = 0.925 d, that we could attribute to the brighter GJ 3039A and the fainter GJ 3039B components, respectively. A comparison of these rotation periods with the period distribution of other β Pictoris members further supports that GJ 3039A is a member of this association. We find that also GJ 3039B could be a member, but the infrared magnitude differences between the two components taken from the literature and the photometric variability, which is found to be comparable in both stars, suggest that GJ 3039B could be a foreground star physically unbound to the primary A component. |
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