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3 results on '"Vasilij G. Shevchenko"'

1. Long-term photometric monitoring of the dwarf planet (136472) Makemake

Author

Pablo Santos-Sanz, Vasilij G. Shevchenko, S. F. Velichko, Vasiliy Rumyantsev, V. R. Ayvazian, Davide Perna, Victor Voropaev, Alexey V. Sergeyev, R. Ya. Inasaridze, Alexander Serebryanskiy, Igor Molotov, Jose Luis Ortiz, Irina Belskaya, Rene Duffard, Audrey Thirouin, Nicolás Morales, Yu. N. Krugly, I. Reva, T. Hromakina, V. Zhuzhunadze, Laboratoire d'études spatiales et d'instrumentation en astrophysique (LESIA (UMR_8109)), Institut national des sciences de l'Univers (INSU - CNRS)-Observatoire de Paris, Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Université Paris Diderot - Paris 7 (UPD7)-Sorbonne Université (SU)-Centre National de la Recherche Scientifique (CNRS), European Commission, Shota Rustaveli National Science Foundation, Ministerio de Ciencia e Innovación (España), Ministry of Education and Science (Kazakhstan), and Ministerio de Ciencia, Innovación y Universidades (España)

Subjects
Absolute magnitude, 010504 meteorology & atmospheric sciences, Kuiper belt objects: (136472) individual: Makemake, media_common.quotation_subject, Dwarf planet, FOS: Physical sciences, Astrophysics, 01 natural sciences, Asymmetry, 0103 physical sciences, 010303 astronomy & astrophysics, ComputingMilieux_MISCELLANEOUS, 0105 earth and related environmental sciences, Spherical shape, media_common, Earth and Planetary Astrophysics (astro-ph.EP), Physics, [PHYS]Physics [physics], photometric [Techniques], Astronomy and Astrophysics, Term (time), Amplitude, (136472) individual: Makemake [Kuiper belt objects], Space and Planetary Science, Satellite, [PHYS.ASTR]Physics [physics]/Astrophysics [astro-ph], Techniques: photometric, Astrophysics - Earth and Planetary Astrophysics
Abstract

Table A.1 is only available at the CDS via anonymous ftp to cdsarc.u-strasbg.fr (130.79.128.5) or via http://cdsarc.u-strasbg.fr/viz-bin/qcat?J/A+A/625/A46, Aims. We studied the rotational properties of the dwarf planet Makemake. Methods. The photometric observations were carried out at different telescopes between 2006 and 2017. Most of the measurements were acquired in BVRI broad-band filters of a standard Johnson-Cousins photometric system. Results. We found that Makemake rotates more slowly than was previously reported. A possible lightcurve asymmetry suggests a double-peaked period of P = 22.8266 ± 0.0001 h. A small peak-to-peak lightcurve amplitude in R-filter A = 0.032 ± 0.005 mag implies an almost spherical shape or near pole-on orientation. We also measured BVRI colours and the R-filter phase-angle slope and revised the absolute magnitudes. The absolute magnitude of Makemake has remained unchanged since its discovery in 2005. No direct evidence of a newly discovered satellite was found in our photometric data; however, we discuss the possible existence of another larger satellite.© ESO 2019, J.L.O., R.D., and P.S.-S acknowledges financial support from the State Agency for Research of the Spanish MCIU through the >Center of Excellence Severo Ochoa> award for the Instituto de Astrofisica de Andalucia (SEV-2017-0709). Funding from MINECO project AYA2017-89637-R is acknowledged. Part of the research leading to these results has received funding from the European Union's Horizon 2020 Research and Innovation Programme, under Grant Agreement no 687378, as part of the project >Small Bodies Near and Far> (SBNAF). R.Ya.I., V.R.A., and V.T.Z. are grateful to the Shota Rustaveli National Science Foundation grant FR-18-1193 for the partial financial support. D.P. has received funding from the European Union's Horizon 2020 research and innovation programme under the Marie Sklodowska-Curie grant agreement n. 664931. I.V.R. and A.V.S. were partly supported by the programme BR05236322 of the Ministry of Education and Science of the Republic of Kazakhstan and the scientific and technical program BR05336383 >Applied scientific research in the field of space activities>.

Published
2019
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2. Opposition effect of Trojan asteroids

Author

I. Slyusarev, Igor Molotov, Yu. N. Krugly, Vasilij G. Shevchenko, Z. Donchev, N. M. Gaftonyuk, Vasilij G. Chiorny, Mansur Ibrahimov, V. Ivanova, Sh. A. Ehgamberdiev, Irina Belskaya, Astronomical Institute of Kharkiv Karazin National University, Laboratoire d'études spatiales et d'instrumentation en astrophysique (LESIA), Université Pierre et Marie Curie - Paris 6 (UPMC)-Institut national des sciences de l'Univers (INSU - CNRS)-Observatoire de Paris, Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Université Paris Diderot - Paris 7 (UPD7)-Centre National de la Recherche Scientifique (CNRS), Pôle Planétologie du LESIA, Laboratoire d'études spatiales et d'instrumentation en astrophysique = Laboratory of Space Studies and Instrumentation in Astrophysics (LESIA), Institut national des sciences de l'Univers (INSU - CNRS)-Observatoire de Paris, Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Sorbonne Université (SU)-Centre National de la Recherche Scientifique (CNRS)-Université Paris Cité (UPCité)-Institut national des sciences de l'Univers (INSU - CNRS)-Observatoire de Paris, Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Sorbonne Université (SU)-Centre National de la Recherche Scientifique (CNRS)-Université Paris Cité (UPCité), Crimean Astrophysical Observatory (CrAO), Rozhen Observatory, Bulgarian Academy of Sciences, Uzbek Academy of Sciences, Ulugh Beg Astronomical Institute, and Keldysh Institute of Applied Mathematics, Russian Academy of Science

Subjects
Physics, Amplitude, Space and Planetary Science, Scattering, Trojan, Asteroid, Phase angle, Astronomy, Astronomy and Astrophysics, Centaur, [PHYS.ASTR]Physics [physics]/Astrophysics [astro-ph]
Abstract

International audience; CCD-photometry of three Jupiter Trojan asteroids were carried out to study their opposition effect. We obtained well-sampled magnitude-phase curves for (588) Achilles, (884) Priamus, and (1143) Odysseus in the maximal attainable phase angle range down to 0.1-0.2°. The magnitude-phase relations have a linear behavior in all observed range of phase angles and do not show any non-linear opposition brightening. We have not found any confident differences between phase slopes measured in B, V and R bands. The values of the measured phase slopes of Trojans are different from available data for Centaurs. They are within the range of phase slopes measured for some low-albedo main belt asteroids, also exhibit a linear behavior down to small phase angles. An absence of non-linear opposition brightening puts constraints on the surface properties of the studied objects, assuming very dark surfaces where single scattering plays dominating role. We also determined the rotation periods, amplitudes, the values of color indexes B-V and V-R, and the absolute magnitudes of these asteroids.

Published
2012
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3. Spin rate distribution of small asteroids

Author

Robert D. Stephens, Štefan Gajdoš, Adrian Galad, François Colas, Petr Pravec, Rui Soles Gonçalves, J. Lecacheux, John Gross, Walter R. Cooney, David Vokrouhlický, Alan W. Harris, N. Gaftonyuk, R. A. Koff, Gianluca Masi, Yu. N. Krugly, Peter Kusnirak, Leonard Kornoš, David Higgins, Vasilij G. Chiorny, Dirk Terrell, R. Durkee, Donald P. Pray, Vasilij G. Shevchenko, Kamil Hornoch, J. G. Ries, Julian Oey, R. R. Dyvig, Vishnu Reddy, Marek Husárik, Jozef Vilagi, Brian D. Warner, Astronomical Institute, Academy of Sciences, Space Science Institute, La Canada, Institute of Astronomy, Faculty of Mathematics and Physics, Charles University, Palmer Divide Observatory, Colorado Springs, Carbuncle Hill Observatory, Hunters Hill Observatory, Leura Observatory, Modra Observatory, Department of Astronomy, Physics of the Earth and Meteorology, Astronomical Institute, Slovak Academy of Sciences, Institute of Astronomy, Kharkiv National University, Crimean Astrophysical Observatory (CrAO), Sonoita Research Observatory, 77 Paint Trail, Sonoita, Goat Mountain Astronomical Research Station, Riverside Astronomical Society, Badlands Observatory, Department of Earth System Science and Policy, University of North Dakota, Grand Forks, Astronomy Department, McDonald Observatory, University of Texas, Institut de Mécanique Céleste et de Calcul des Ephémérides (IMCCE), Université Pierre et Marie Curie - Paris 6 (UPMC)-Institut national des sciences de l'Univers (INSU - CNRS)-Observatoire de Paris, Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Université de Lille-Centre National de la Recherche Scientifique (CNRS), Laboratoire d'études spatiales et d'instrumentation en astrophysique (LESIA), Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Université Paris Diderot - Paris 7 (UPD7)-Centre National de la Recherche Scientifique (CNRS), Pôle Planétologie du LESIA, Laboratoire d'études spatiales et d'instrumentation en astrophysique = Laboratory of Space Studies and Instrumentation in Astrophysics (LESIA), Institut national des sciences de l'Univers (INSU - CNRS)-Observatoire de Paris, Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Sorbonne Université (SU)-Centre National de la Recherche Scientifique (CNRS)-Université Paris Cité (UPCité)-Institut national des sciences de l'Univers (INSU - CNRS)-Observatoire de Paris, Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Sorbonne Université (SU)-Centre National de la Recherche Scientifique (CNRS)-Université Paris Cité (UPCité), Shed of Science Observatory, Bellatrix Astronomical Observatory, Antelope Hills Observatory, 980 Antelope Drive West, Bennett, and Observatório Astronómico de Linhaceira

Subjects
Physics, Solar System, education.field_of_study, Near-Earth object, Population, Astronomy, Astronomy and Astrophysics, Photometry (optics), Space and Planetary Science, Asteroid, Magnitude (astronomy), education, [PHYS.ASTR]Physics [physics]/Astrophysics [astro-ph], Residence time (statistics), Spin-½
Abstract

The spin rate distribution of main belt/Mars crossing (MB/MC) asteroids with diameters 3–15 km is uniform in the range from f = 1 to 9.5 d−1, and there is an excess of slow rotators with f 1 d−1. The observed distribution appears to be controlled by the Yarkovsky–O'Keefe–Radzievskii–Paddack (YORP) effect. The magnitude of the excess of slow rotators is related to the residence time of slowed down asteroids in the excess and the rate of spin rate change outside the excess. We estimated a median YORP spin rate change of ≈ 0.022 d −1 / Myr for asteroids in our sample (i.e., a median time in which the spin rate changes by 1 d−1 is ≈ 45 Myr ), thus the residence time of slowed down asteroids in the excess is ≈ 110 Myr . The spin rate distribution of near-Earth asteroids (NEAs) with sizes in the range 0.2–3 km (∼5 times smaller in median diameter than the MB/MC asteroids sample) shows a similar excess of slow rotators, but there is also a concentration of NEAs at fast spin rates with f = 9 – 10 d −1 . The concentration at fast spin rates is correlated with a narrower distribution of spin rates of primaries of binary systems among NEAs; the difference may be due to the apparently more evolved population of binaries among MB/MC asteroids.

Published
2008
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