Volume 645, January 2021
|Number of page(s)||16|
|Section||Celestial mechanics and astrometry|
|Published online||15 January 2021|
Dynamics of charged dust in the orbit of Venus
School of Astronomy and Space Science, Nanjing University,
163 Xianlin Avenue,
2 Institute of Astrophysics, University of Vienna, Türkenschanzstrasse 17, 1180 Vienna, Austria
3 Key Laboratory of Modern Astronomy and Astrophysics in Ministry of Education, Nanjing University, Nanjing 210046, PR China
4 Space Research Institute, Austrian Academy of Sciences, Schmiedlstrasse 6, 8042 Graz, Austria
5 Department of Mathematics, University of Rome Tor Vergata, Via della Ricerca Scientifica 1, 00133 Roma, Italy
6 Faculty of Mathematics, ‘Al. I. Cuza’ University of Iasi, Bd. Carol I., 11, 7000506 Iasi, Romania
7 Institute of Space Astronomy and Extraterrestial Exploration (NJU & CAST), Nanjing 210046, PR China
Accepted: 4 December 2020
We study the dynamics of co-orbital dust in the inner Solar System, that is, the role of the solar radiation pressure, the Poynting-Robertson effect, the solar wind, and the interplanetary magnetic field, on the location, width, and stability of resonant motion of charged and micron-sized dust grains situated in the 1:1 mean motion resonance with Venus. We find deviations and asymmetry between L4 and L5 in the locations of the libration centers and libration width caused by nongravitational effects with analytical and numerical methods. The triangular Lagrangian points become unstable when solar radiation pressure, the Poynting-Robertson effect, and solar wind drag are considered. The Lorentz force could further destabilize the orbits, especially for small dust particles. We also compare the circular and/or elliptic restricted three-body model and a more complete model that includes all planets.
Key words: zodiacal dust / methods: analytical / methods: numerical / planets and satellites: individual: Venus / Sun: heliosphere / chaos
© ESO 2021
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