Long-term orbital and rotational motions of Ceres and Vesta
International audience Context. The dwarf planet Ceres and the asteroid Vesta have been studied by the Dawn space mission. They are the two heaviest bodies of the main asteroid belt and have different characteristics. Notably, Vesta appears to be dry and inactive with two large basins at its south p...
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ftccsdartic:oai:HAL:hal-03009222v1 2023-05-15T18:23:08+02:00 Long-term orbital and rotational motions of Ceres and Vesta Vaillant, T. Laskar, J. Rambaux, N. Gastineau, M. Institut de Mécanique Céleste et de Calcul des Ephémérides (IMCCE) 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-Sorbonne Université (SU)-Centre National de la Recherche Scientifique (CNRS) 2019 https://hal.archives-ouvertes.fr/hal-03009222 https://hal.archives-ouvertes.fr/hal-03009222/document https://hal.archives-ouvertes.fr/hal-03009222/file/aa33342-18.pdf https://doi.org/10.1051/0004-6361/201833342 en eng HAL CCSD EDP Sciences info:eu-repo/semantics/altIdentifier/arxiv/1808.10384 info:eu-repo/semantics/altIdentifier/doi/10.1051/0004-6361/201833342 hal-03009222 https://hal.archives-ouvertes.fr/hal-03009222 https://hal.archives-ouvertes.fr/hal-03009222/document https://hal.archives-ouvertes.fr/hal-03009222/file/aa33342-18.pdf ARXIV: 1808.10384 BIBCODE: 2019A&A.622A.95V doi:10.1051/0004-6361/201833342 info:eu-repo/semantics/OpenAccess ISSN: 0004-6361 EISSN: 1432-0756 Astronomy and Astrophysics - A&A https://hal.archives-ouvertes.fr/hal-03009222 Astronomy and Astrophysics - A&A, EDP Sciences, 2019, 622, pp.A95. ⟨10.1051/0004-6361/201833342⟩ celestial mechanics minor planets asteroids: individual: Vesta asteroids: individual: Ceres planets and satellites: dynamical evolution and stability [PHYS.ASTR]Physics [physics]/Astrophysics [astro-ph] [PHYS]Physics [physics] info:eu-repo/semantics/article Journal articles 2019 ftccsdartic https://doi.org/10.1051/0004-6361/201833342 2021-12-05T00:55:09Z International audience Context. The dwarf planet Ceres and the asteroid Vesta have been studied by the Dawn space mission. They are the two heaviest bodies of the main asteroid belt and have different characteristics. Notably, Vesta appears to be dry and inactive with two large basins at its south pole. Ceres is an ice-rich body with signs of cryovolcanic activity.Aims. The aim of this paper is to determine the obliquity variations of Ceres and Vesta and to study their rotational stability.Methods. The orbital and rotational motions have been integrated by symplectic integration. The rotational stability has been studied by integrating secular equations and by computing the diffusion of the precession frequency.Results. The obliquity variations of Ceres over [−20 : 0] Myr are between 2° and 20° and the obliquity variations of Vesta are between 21° and 45°. The two giant impacts suffered by Vesta modified the precession constant and could have put Vesta closer to the resonance with the orbital frequency 2s6 − sV. Given the uncertainty on the polar moment of inertia, the present Vesta could be in this resonance where the obliquity variations can vary between 17° and 48°.Conclusions. Although Ceres and Vesta have precession frequencies close to the secular orbital frequencies of the inner planets, their long-term rotations are relatively stable. The perturbations of Jupiter and Saturn dominate the secular orbital dynamics of Ceres and Vesta and the perturbations of the inner planets are much weaker. The secular resonances with the inner planets also have smaller widths and do not overlap, contrary to the case of the inner planets. Article in Journal/Newspaper South pole Archive ouverte HAL (Hyper Article en Ligne, CCSD - Centre pour la Communication Scientifique Directe) Jupiter ENVELOPE(101.133,101.133,-66.117,-66.117) South Pole Astronomy & Astrophysics 622 A95 |
institution |
Open Polar |
collection |
Archive ouverte HAL (Hyper Article en Ligne, CCSD - Centre pour la Communication Scientifique Directe) |
op_collection_id |
ftccsdartic |
language |
English |
topic |
celestial mechanics minor planets asteroids: individual: Vesta asteroids: individual: Ceres planets and satellites: dynamical evolution and stability [PHYS.ASTR]Physics [physics]/Astrophysics [astro-ph] [PHYS]Physics [physics] |
spellingShingle |
celestial mechanics minor planets asteroids: individual: Vesta asteroids: individual: Ceres planets and satellites: dynamical evolution and stability [PHYS.ASTR]Physics [physics]/Astrophysics [astro-ph] [PHYS]Physics [physics] Vaillant, T. Laskar, J. Rambaux, N. Gastineau, M. Long-term orbital and rotational motions of Ceres and Vesta |
topic_facet |
celestial mechanics minor planets asteroids: individual: Vesta asteroids: individual: Ceres planets and satellites: dynamical evolution and stability [PHYS.ASTR]Physics [physics]/Astrophysics [astro-ph] [PHYS]Physics [physics] |
description |
International audience Context. The dwarf planet Ceres and the asteroid Vesta have been studied by the Dawn space mission. They are the two heaviest bodies of the main asteroid belt and have different characteristics. Notably, Vesta appears to be dry and inactive with two large basins at its south pole. Ceres is an ice-rich body with signs of cryovolcanic activity.Aims. The aim of this paper is to determine the obliquity variations of Ceres and Vesta and to study their rotational stability.Methods. The orbital and rotational motions have been integrated by symplectic integration. The rotational stability has been studied by integrating secular equations and by computing the diffusion of the precession frequency.Results. The obliquity variations of Ceres over [−20 : 0] Myr are between 2° and 20° and the obliquity variations of Vesta are between 21° and 45°. The two giant impacts suffered by Vesta modified the precession constant and could have put Vesta closer to the resonance with the orbital frequency 2s6 − sV. Given the uncertainty on the polar moment of inertia, the present Vesta could be in this resonance where the obliquity variations can vary between 17° and 48°.Conclusions. Although Ceres and Vesta have precession frequencies close to the secular orbital frequencies of the inner planets, their long-term rotations are relatively stable. The perturbations of Jupiter and Saturn dominate the secular orbital dynamics of Ceres and Vesta and the perturbations of the inner planets are much weaker. The secular resonances with the inner planets also have smaller widths and do not overlap, contrary to the case of the inner planets. |
author2 |
Institut de Mécanique Céleste et de Calcul des Ephémérides (IMCCE) 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-Sorbonne Université (SU)-Centre National de la Recherche Scientifique (CNRS) |
format |
Article in Journal/Newspaper |
author |
Vaillant, T. Laskar, J. Rambaux, N. Gastineau, M. |
author_facet |
Vaillant, T. Laskar, J. Rambaux, N. Gastineau, M. |
author_sort |
Vaillant, T. |
title |
Long-term orbital and rotational motions of Ceres and Vesta |
title_short |
Long-term orbital and rotational motions of Ceres and Vesta |
title_full |
Long-term orbital and rotational motions of Ceres and Vesta |
title_fullStr |
Long-term orbital and rotational motions of Ceres and Vesta |
title_full_unstemmed |
Long-term orbital and rotational motions of Ceres and Vesta |
title_sort |
long-term orbital and rotational motions of ceres and vesta |
publisher |
HAL CCSD |
publishDate |
2019 |
url |
https://hal.archives-ouvertes.fr/hal-03009222 https://hal.archives-ouvertes.fr/hal-03009222/document https://hal.archives-ouvertes.fr/hal-03009222/file/aa33342-18.pdf https://doi.org/10.1051/0004-6361/201833342 |
long_lat |
ENVELOPE(101.133,101.133,-66.117,-66.117) |
geographic |
Jupiter South Pole |
geographic_facet |
Jupiter South Pole |
genre |
South pole |
genre_facet |
South pole |
op_source |
ISSN: 0004-6361 EISSN: 1432-0756 Astronomy and Astrophysics - A&A https://hal.archives-ouvertes.fr/hal-03009222 Astronomy and Astrophysics - A&A, EDP Sciences, 2019, 622, pp.A95. ⟨10.1051/0004-6361/201833342⟩ |
op_relation |
info:eu-repo/semantics/altIdentifier/arxiv/1808.10384 info:eu-repo/semantics/altIdentifier/doi/10.1051/0004-6361/201833342 hal-03009222 https://hal.archives-ouvertes.fr/hal-03009222 https://hal.archives-ouvertes.fr/hal-03009222/document https://hal.archives-ouvertes.fr/hal-03009222/file/aa33342-18.pdf ARXIV: 1808.10384 BIBCODE: 2019A&A.622A.95V doi:10.1051/0004-6361/201833342 |
op_rights |
info:eu-repo/semantics/OpenAccess |
op_doi |
https://doi.org/10.1051/0004-6361/201833342 |
container_title |
Astronomy & Astrophysics |
container_volume |
622 |
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A95 |
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1766202565452627968 |