Stability of prograde and retrograde planets in circular binary systems
Open accessAbstract
We investigate the stability of prograde versus retrograde planets in circular binary systems using numerical simulations. We show that retrograde planets are stable up to distances closer to the perturber than prograde planets. We develop an analytical model to compute the prograde and retrograde mean motion resonances’ locations and separatrices. We show that instability is due to single resonance forcing, or caused by nearby resonances’ overlap. We validate our results regarding the role of single resonances and resonances’ overlap on orbit stability, by computing surfaces of section of the circular restricted three-body problem. We conclude that the observed enhanced stability of retrograde planets with respect to prograde planets is due to essential differences between the phase-space topology of retrograde versus prograde resonances (at p/q mean motion ratio, the prograde resonance is of order p−q while the retrograde resonance is of order p+q).
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Retrograde ring systems are typically 1.4 times the size of prograde ring systems.
“Retrograde ring systems are typically 1.4 times the size of prograde ring systems, consistent with similar results from other simulations (Toomre & Toomre 1972;Morais & Giuppone 2012).”
From Constraints on the size and dynamics of the J1407b ring system (2016) · cites this paper as Morais & Giuppone 2012
The Abstract (p. 1) reports that retrograde planets in circular binary systems remain stable closer to the perturber than prograde planets, supporting the qualitative comparison. The paper studies planetary orbits, not ring-system sizes, and the passages do not establish a typical 1.4-to-1 size ratio. (LLM, conf=0.88)
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Research works printed but not linked: 3
- Beauge C., Nesvorny D., 2011, ArXiv e-prints
- Murray C. D., Dermott S. F., 1999, Solar system dynamics. Cambridge University Press
- Peale S. J., 1976, Annual Review of Astronomy & Astrophysics, 14, 215
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Constraints on the size and dynamics of the J1407b ring system
Rieder, S., & Kenworthy, M. A. (2016) · Astronomy & Astrophysics · doi:10.1051/0004-6361/201629567 · Cited by 23 · see citing works
“This is in agreement with classical results from e.g. Toomre & Toomre (1972), who studied similar interactions on a galaxy scale, and Morais & Giuppone (2012), who studied 3-body systems on planetary scale.”
ResultInfluential
- Authors
- Morais, M. H. M., & Giuppone, C. A.
- Affiliations
- University of Aveiro (PT)
- Corresponding author
- Morais, M. H. M.
- ORCID
- Giuppone, C. A.
- Venue
- Monthly Notices of the Royal Astronomical Society
- Publisher
- Oxford University Press (OUP)
- Published
- 2012-05-29
- Volume
- 424
- Issue
- 1
- Pages
- 52-64
- ISSN
- 0035-8711 (ISSN-L)
- OpenAlex
- W1941902670
- Cited by
- 92
- References
- 0
- Citations by year
- 2026: 1 · 2025: 6 · 2024: 2 · 2023: 4 · 2022: 1 · 2021: 8 · 2020: 7 · 2019: 4 · 2018: 32 · 2017: 6 · 2016: 5 · 2015: 4 · 2014: 3 · 2013: 5 · 2012: 1
- FWCI
- 2.28
- Type
- journal article
- Language
- en
- Open access
- green
- arxiv.org
- Locations
- Monthly Notices of the Royal Astronomical Society (publishedVersion)
- arXiv (Cornell University) (submittedVersion)
- arXiv (Cornell University)
- Topics
- Physical Sciences › Physics and Astronomy › Astronomy and Astrophysics › Stellar, planetary, and galactic studies
- Physical Sciences › Physics and Astronomy › Astronomy and Astrophysics › Astro and Planetary Science
- Physical Sciences › Engineering › Aerospace Engineering › Spacecraft Dynamics and Control
- Keywords
- binary stars, orbital stability, mean motion resonance, overlapping resonances, circular restricted three-body problem, separatrices, phase space topology
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