Issue |
A&A
Volume 689, September 2024
|
|
---|---|---|
Article Number | A4 | |
Number of page(s) | 24 | |
Section | Celestial mechanics and astrometry | |
DOI | https://doi.org/10.1051/0004-6361/202449770 | |
Published online | 03 September 2024 |
A perturbative treatment of the Yarkovsky-driven drifts in the 2:1 mean motion resonance
1
School of Astronomy and Space Science, Nanjing University
Nanjing
210023,
PR China
e-mail: houxiyun@nju.edu.cn
2
Institute of Space Environment and Astrodynamics, Nanjing University,
Nanjing
210023,
PR China
3
Key Laboratory of Modern Astronomy and Astrophysics, Ministry of Education,
Nanjing
210023,
PR China
Received:
28
February
2024
Accepted:
5
July
2024
Aims. Our aim is to gain a qualitative understanding as well as to perform a quantitative analysis of the interplay between the Yarkovsky effect and the Jovian 2:1 mean motion resonance under the planar elliptic restricted three-body problem.
Methods. We adopted the semi-analytical perturbation method valid for arbitrary eccentricity to obtain the resonance structures inside the Jovian 2:1 resonance. We averaged the Yarkovsky force so it could be applied to the integrable approximations for the 2:1 resonance and the ν5 secular resonance. The rates of Yarkovsky-driven drifts in the action space were derived from the quasi-integrable approximations perturbed by the averaged Yarkovsky force. Pseudo-proper elements of test particles inside the 2:1 resonance were computed using N-body simulations incorporated with the Yarkovsky effect to verify the semi-analytical results.
Results. In the planar elliptic restricted model, we identified two main types of systematic drifts in the action space: (Type I) for orbits not trapped in the ν5 resonance, the footprints are parallel to the resonance curve of the stable center of the 2:1 resonance; (Type II) for orbits trapped in the ν5 resonance, the footprints are parallel to the resonance curve of the stable center of the ν5 resonance. Using the semi-analytical perturbation method, a vector field in the action space corresponding to the two types of systematic drifts was derived. The Type I drift with small eccentricities and small libration amplitudes of 2:1 resonance can be modeled by a harmonic oscillator with a slowly varying parameter, for which an analytical treatment using the adiabatic invariant theory was carried out.
Key words: celestial mechanics
© The Authors 2024
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