Skip to content
DraconiticResearch
Search Sources API
197,693 studies31 sourcesUpdated 49 min ago
Peer-reviewedCC BY 4.0Monthly Notices of the Royal Astronomical Society

Dynamics around non-spherical symmetric bodies–III. The case of a spherical body with a crater

  • P V S Soares1
  • G Madeira2
  • S M Giuliatti Winter1
  • T Ribeiro1
  • O C Winter1
  1. 1Grupo de Dinâmica Orbital e Planetologia (GDOP), São Paulo State University-UNESP , Guaratinguetá, SP, CEP 12516-410 ,
  2. 2Observatório Nacional/MCTI , R. General José Cristino 77, CEP 20921-400, RJ ,
Open at sourcePDFDOICite

Abstract

Motivated by the peculiar features of the trans-Neptunian object (TNO) Máni and the discovery of ring systems around Centaurs and trans-Neptunian bodies, we investigate the stability of particles around a small irregular body hosting a deep equatorial crater. This study is the third contribution in a sequence devoted to the dynamics around non-spherically symmetric bodies. Using Máni as a reference model, whose crater depth exceeds 10 per cent of its radius, we map the system stability through complementary methods: Poincaré surfaces of section (PSS), survival maps, and the finite-time Lyapunov exponent (FTLE). In the nominal case, the 1 : 1, 2 : 1, 3 : 1, and 4 : 1 spin-orbit resonances (SORs) are consistently identified by all techniques. The prominent 3 : 1 SOR exhibits a bifurcated structure at high eccentricities, matching structural transitions observed at lower Jacobi constant values in the PSSs. Increasing the rotation rate (λ) and crater mass ratio (μ) enlarges resonance widths and promotes overlap, making the 2 : 1 and 4 : 1 SORs progressively dominant. Lower rotation rates allow stable trajectories to persist at higher eccentricities, whereas the 1 : 1 SOR is highly sensitive to stronger perturbations and disappears in the most extreme cases. In contrast to mass-anomaly models, which can clear the region interior to the 2 : 1 SOR, the crater configuration considered here preserves stable regions in this vicinity, suggesting alternative scenarios for the formation and maintenance of debris structures around irregular minor bodies.

Related

  1. Spherical Accretion onto Konoplya Zhidenko Black Holes: Sonic Point Analysis and Fluid Dynamics
    M H Waheed, M Z A Moughal
    arXivPreprintCC BY 4.0Full textHigh-energy astrophysicsGravitation & general relativityarXiv
  2. Fast partial-sky spherical harmonic transforms
    J. Carron, M. Reinecke
    Astronomy & AstrophysicsPeer-reviewedPublisher termsCosmologyCrossref
  3. Probing modified gravity with compensated spherical regions: Broken Birkhoff locality and a scale-dependent growth rate
    P. de Fromont, J.-M. Alimi
    Astronomy & AstrophysicsPeer-reviewedPublisher termsCosmologyCrossref
  4. Disruption limits around triaxial bodies and implications for ring-bearing minor bodies
    Gustavo Madeira, T. F. L. L. Pinheiro
    arXivPreprintCC BY-NC-ND 4.0Full textPlanetary science & exoplanetsarXiv
  5. Continuous Learning of Gravity Field Irregularities Around Small Bodies via Neural Hamiltonian ODEs
    Giacomo Acciarini, Dario Izzo
    arXivPreprintCC BY 4.0Full textInstrumentation & methodsPlanetary science & exoplanetsarXiv

Cite

BibTeXRIS
BibTeX
@article{soares2026dynamics,
  title = {{Dynamics around non-spherical symmetric bodies–III. The case of a spherical body with a crater}},
  author = {P V S Soares and G Madeira and S M Giuliatti Winter and T Ribeiro and O C Winter},
  journal = {Monthly Notices of the Royal Astronomical Society},
  year = {2026},
  month = oct,
  doi = {10.1093/mnras/stag1900},
  url = {https://academic.oup.com/mnras/article/doi/10.1093/mnras/stag1900/8876088},
  note = {CC BY 4.0},
}
RIS
TY  - JOUR
TI  - Dynamics around non-spherical symmetric bodies–III. The case of a spherical body with a crater
AU  - P V S Soares
AU  - G Madeira
AU  - S M Giuliatti Winter
AU  - T Ribeiro
AU  - O C Winter
PY  - 2026
DA  - 2026/10/07
JO  - Monthly Notices of the Royal Astronomical Society
DO  - 10.1093/mnras/stag1900
UR  - https://academic.oup.com/mnras/article/doi/10.1093/mnras/stag1900/8876088
AB  - Motivated by the peculiar features of the trans-Neptunian object (TNO) Máni and the discovery of ring systems around Centaurs and trans-Neptunian bodies, we investigate the stability of particles around a small irregular body hosting a deep equatorial crater. This study is the third contribution in a sequence devoted to the dynamics around non-spherically symmetric bodies. Using Máni as a reference model, whose crater depth exceeds 10 per cent of its radius, we map the system stability through complementary methods: Poincaré surfaces of section (PSS), survival maps, and the finite-time Lyapunov exponent (FTLE). In the nominal case, the 1 : 1, 2 : 1, 3 : 1, and 4 : 1 spin-orbit resonances (SORs) are consistently identified by all techniques. The prominent 3 : 1 SOR exhibits a bifurcated structure at high eccentricities, matching structural transitions observed at lower Jacobi constant values in the PSSs. Increasing the rotation rate (λ) and crater mass ratio (μ) enlarges resonance widths and promotes overlap, making the 2 : 1 and 4 : 1 SORs progressively dominant. Lower rotation rates allow stable trajectories to persist at higher eccentricities, whereas the 1 : 1 SOR is highly sensitive to stronger perturbations and disappears in the most extreme cases. In contrast to mass-anomaly models, which can clear the region interior to the 2 : 1 SOR, the crater configuration considered here preserves stable regions in this vicinity, suggesting alternative scenarios for the formation and maintenance of debris structures around irregular minor bodies.
SN  - 0035-8711
SN  - 1365-2966
ER  -