2018/03/12 by E. Forgács‐Dajka, E. Forgács-Dajka, Zs. Sándor +1 · 26 citations
Physics and Astronomy · #A priori and a posteriori #Asteroid #Astro and Planetary Science #Astronomy #Astrophysics #Astrophysics and Star Formation Studies #Classical mechanics #Exoplanet #Jupiter (rocket family) #Mean motion #Motion (physics) #Neptune #Physics #Planet #Resonance (particle physics) #Solar System #Spacecraft #Stellar, planetary, and galactic studies #astro-ph.EP
paper · pdf · doi:10.1093/mnras/sty641
published in Monthly Notices of the Royal Astronomical Society 477(3), 3383-3389 (Oxford University Press) · 7 pages, 13 figures, accepted by Monthly Notices of the Royal Astronomical Society
openalex publication_date 2018/03/12 · arxiv created 2018/03/20 · arxiv updated 2018/03/21 · openalex created_date 2025/10/10 · openalex updated_date 2026/08/05
The identification of mean motion resonances in exoplanetary systems or in the Solar system might be cumbersome when several planets and large number of smaller bodies are to be considered. Based on the geometrical meaning of the resonance variable, an efficient method is introduced and described here, by which mean motion resonances can be easily find without any a priori knowledge on them. The efficiency of this method is clearly demonstrated by using known exoplanets engaged in mean motion resonances, and also some members of different families of asteroids and Kuiper belt objects being in mean motion resonances with Jupiter and Neptune, respectively.