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Optical observations of NEA 3200 Phaethon (1983 TB) during the 2017 apparition

M.-J. KimKorea Astronomy and Space Science Institute, 776, Daedeokdae-ro, Yuseong-gu, Daejeon 34055, KoreaH.-J. LeeChungbuk National University, 1 Chungdae-ro, Seowon-gu, Cheongju, Chungbuk 28644, KoreaS.-M. LeeChungbuk National University, 1 Chungdae-ro, Seowon-gu, Cheongju, Chungbuk 28644, KoreaD.-H. KimKorea Astronomy and Space Science Institute, 776, Daedeokdae-ro, Yuseong-gu, Daejeon 34055, KoreaF. YoshidaPlanetary Exploration Research Center, Chiba Institute of Technology, 2-17-1 Tsudanuma, Narashino, Chiba 275-0016, JapanP. BartczakAstronomical Observatory Institute, Faculty of Physics, Adam Mickiewicz University, Słoneczna 36, 60-286 Poznań, PolandG. DudzińskiAstronomical Observatory Institute, Faculty of Physics, Adam Mickiewicz University, Słoneczna 36, 60-286 Poznań, PolandJ. ParkKorea Astronomy and Space Science Institute, 776, Daedeokdae-ro, Yuseong-gu, Daejeon 34055, KoreaY.-J. ChoiKorea Astronomy and Space Science Institute, 776, Daedeokdae-ro, Yuseong-gu, Daejeon 34055, KoreaH.-K. MoonKorea Astronomy and Space Science Institute, 776, Daedeokdae-ro, Yuseong-gu, Daejeon 34055, KoreaH.-S. YimKorea Astronomy and Space Science Institute, 776, Daedeokdae-ro, Yuseong-gu, Daejeon 34055, KoreaJ. ChoiKorea Astronomy and Space Science Institute, 776, Daedeokdae-ro, Yuseong-gu, Daejeon 34055, KoreaE.-J. ChoiKorea Astronomy and Space Science Institute, 776, Daedeokdae-ro, Yuseong-gu, Daejeon 34055, KoreaJ.-N. YoonChungbuk National University Observatory, 802-3 Euntan-ri, Jincheon-gun, Chungcheongbuk-do, KoreaA. SerebryanskiyFesenkov Astrophysical Institute, Observatory 23, 050020 Almaty, KazakhstanM. KrugovFesenkov Astrophysical Institute, Observatory 23, 050020 Almaty, KazakhstanI. RevaFesenkov Astrophysical Institute, Observatory 23, 050020 Almaty, KazakhstanK. E. ErgashevUlugh Beg Astronomical Institute of the Uzbekistan Academy of Sciences, 33 Astronomicheskaya str., Tashkent, 100052, UzbekistanO. BurkhonovUlugh Beg Astronomical Institute of the Uzbekistan Academy of Sciences, 33 Astronomicheskaya str., Tashkent, 100052, UzbekistanSh. A. EhgamberdievUlugh Beg Astronomical Institute of the Uzbekistan Academy of Sciences, 33 Astronomicheskaya str., Tashkent, 100052, UzbekistanY. TurayevUlugh Beg Astronomical Institute of the Uzbekistan Academy of Sciences, 33 Astronomicheskaya str., Tashkent, 100052, UzbekistanZ.-Y. LinInstitute of Astronomy, National Central University, No. 300, Zhongda Rd., Zhongli Dist., Taoyuan City 32001, TaiwanT. AraiPlanetary Exploration Research Center, Chiba Institute of Technology, 2-17-1 Tsudanuma, Narashino, Chiba 275-0016, JapanK. OhtsukaT. ItoNational Astronomical Observatory of Japan, Osawa 2-21-1, Mitaka, Tokyo 181-8588, JapanS. UrakawaJapan Spaceguard Association, Bisei Spaceguard Center, 1716-3 Okura, Bisei-cho, Ibara, Okayama 714-1411, JapanM. IshiguroSeoul National University, 1 Gwanak-ro, Gwanak-gu, Seoul 08826, Korea

Astronomy and Astrophysicsjournal2018en

ABI

Аннотация

Context. The near-Earth asteroid 3200 Phaethon (1983 TB) is an attractive object not only from a scientific viewpoint but also because of JAXA’s DESTINY + target. The rotational lightcurve and spin properties were investigated based on the data obtained in the ground-based observation campaign of Phaethon. Aims. We aim to refine the lightcurves and shape model of Phaethon using all available lightcurve datasets obtained via optical observation, as well as our time-series observation data from the 2017 apparition. Methods. Using eight 12-m telescopes and an optical imager, we acquired the optical lightcurves and derived the spin parameters of Phaethon. We applied the lightcurve inversion method and SAGE algorithm to deduce the convex and non-convex shape model and pole orientations. Results. We analysed the optical lightcurve of Phaethon and derived a synodic and a sidereal rotational periods of 3.6039 h, with an axis ratio of a ∕ b = 1.07. The ecliptic longitude ( λ p ) and latitude ( β p ) of the pole orientation were determined as (308°, −52°) and (322°, −40°) via two independent methods. A non-convex model from the SAGE method, which exhibits a concavity feature, is also presented.

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Мавзулар

Astro and Planetary Science Planetary Science and Exploration High-pressure geophysics and materials

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DOI: 10.1051/0004-6361/201833593

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