scholarly journals Instabilities in multiplanet circumbinary systems

2019 ◽  
Vol 487 (3) ◽  
pp. 3288-3304 ◽  
Author(s):  
Adam P Sutherland ◽  
Kaitlin M Kratter
Keyword(s):  
Mean Motion Resonances ◽  
Migration Rates ◽  
Mean Motion ◽  
Planet Migration ◽  
Circumbinary Planets

ABSTRACT The majority of the discovered transiting circumbinary planets are located very near the innermost stable orbits permitted, raising questions about the origins of planets in such perturbed environments. Most favoured formation scenarios invoke formation at larger distances and subsequent migration to their current locations. Disc-driven planet migration in multiplanet systems is likely to trap planets in mean motion resonances and drive planets inwards into regions of larger dynamical perturbations from the binary. We demonstrate how planet–planet resonances can interact with the binary through secular forcing and mean-motion resonances, driving chaos in the system. We show how this chaos will shape the architecture of circumbinary systems, with specific applications to Kepler 47 and the Pluto–Charon system, limiting maximum possible stable eccentricities and indicating what resonances are likely to exist. We are also able to constrain the minimum migration rates of resonant circumbinary planets.

scholarly journals Hamiltonian model of capture into mean motion resonance

2010 ◽  
Vol 6 (S276) ◽  
pp. 300-303 ◽  
Author(s):  
Alexander J. Mustill ◽  
Mark C. Wyatt
Keyword(s):  
Extrasolar Planets ◽  
Kuiper Belt ◽  
Mean Motion Resonances ◽  
Migration Rates ◽  
Mean Motion ◽  
Hamiltonian Model ◽  
Planet Migration ◽  
High Migration ◽  
Relative Migration ◽  
Probability Of Capture

AbstractMean motion resonances are a common feature of both our own Solar System and of extrasolar planetary systems. Bodies can be trapped in resonance when their orbital semi-major axes change, for instance when they migrate through a protoplanetary disc. We use a Hamiltonian model to thoroughly investigate the capture behaviour for first and second order resonances. Using this method, all resonances of the same order can be described by one equation, with applications to specific resonances by appropriate scaling. We focus on the limit where one body is a massless test particle and the other a massive planet. We quantify how the the probability of capture into a resonance depends on the relative migration rate of the planet and particle, and the particle's eccentricity. Resonant capture fails for high migration rates, and has decreasing probability for higher eccentricities, although for certain migration rates, capture probability peaks at a finite eccentricity. We also calculate libration amplitudes and the offset of the libration centres for captured particles, and the change in eccentricity if capture does not occur. Libration amplitudes are higher for larger initial eccentricity. The model allows for a complete description of a particle's behaviour as it successively encounters several resonances. The model is applicable to many scenarios, including (i) Planet migration through gas discs trapping other planets or planetesimals in resonances; (ii) Planet migration through a debris disc; (iii) Dust migration through PR drag. The Hamiltonian model will allow quick interpretation of the resonant properties of extrasolar planets and Kuiper Belt Objects, and will allow synthetic images of debris disc structures to be quickly generated, which will be useful for predicting and interpreting disc images made with ALMA, Darwin/TPF or similar missions. Full details can be found in Mustill & Wyatt (2011).

scholarly journals Motion of dust in mean motion resonances with planets

2009 ◽  
Vol 103 (4) ◽  
pp. 343-364 ◽  
Author(s):  
Pavol Pástor ◽  
Jozef Klačka ◽  
Ladislav Kómar
Keyword(s):  
Mean Motion Resonances ◽  
Mean Motion

scholarly journals Planets in Mean-Motion Resonances and the System Around HD45364

2018 ◽  
pp. 2693-2711
Author(s):  
Alexandre C. M. Correia ◽  
Jean-Baptiste Delisle ◽  
Jacques Laskar
Keyword(s):  
Mean Motion Resonances ◽  
Mean Motion

scholarly journals Dynamics of Comets

1992 ◽  
Vol 152 ◽  
pp. 255-268 ◽  
Author(s):  
A. Carusi ◽  
G.B. Valsecchi
Keyword(s):  
Molecular Clouds ◽  
Vertical Component ◽  
The Sun ◽  
Giant Molecular Clouds ◽  
Mean Motion Resonances ◽  
Galactic Field ◽  
Mean Motion ◽  
Short Period ◽  
Gravitational Processes

The gravitational processes affecting the dynamics of comets are reviewed. At great distances from the Sun the motion of comets is primarily affected by the vertical component of the galactic field, as well as by encounters with stars and giant molecular clouds. When comets move in the region of the planets, encounters with these can strongly affect their motion. A good fraction of all periodic comets spend some time in temporary libration about mean motion resonances with Jupiter; some comets can be captured by this planet as temporary satellites. Finally, there is a small number of objects with orbital characteristics quite different from those of all other short-period comets.

Mean Motion Resonances in the Trans-neptunian Region

Icarus ◽  
2000 ◽  
Vol 148 (1) ◽  
pp. 282-300 ◽  
Author(s):  
D. Nesvorný ◽  
F. Roig
Keyword(s):  
Mean Motion Resonances ◽  
Mean Motion

scholarly journals Orbital evolution of Saturn’s satellites due to the interaction between the moons and the massive rings

2020 ◽  
Vol 640 ◽  
pp. L15
Author(s):  
Ayano Nakajima ◽  
Shigeru Ida ◽  
Yota Ishigaki
Keyword(s):  
Orbital Evolution ◽  
The Self ◽  
Mean Motion Resonances ◽  
First Order ◽  
Mean Motion ◽  
Saturn’S Satellites ◽  
Orbital Configuration ◽  
Self Gravity ◽  
Spiral Arm ◽  
Orbital Migration

Context. Saturn’s mid-sized moons (satellites) have a puzzling orbital configuration with trapping in mean-motion resonances with every-other pairs (Mimas-Tethys 4:2 and Enceladus-Dione 2:1). To reproduce their current orbital configuration on the basis of a recent model of satellite formation from a hypothetical ancient massive ring, adjacent pairs must pass first-order mean-motion resonances without being trapped. Aims. The trapping could be avoided by fast orbital migration and/or excitation of the satellite’s eccentricity caused by gravitational interactions between the satellites and the rings (the disk), which are still unknown. In our research we investigate the satellite orbital evolution due to interactions with the disk through full N-body simulations. Methods. We performed global high-resolution N-body simulations of a self-gravitating particle disk interacting with a single satellite. We used N ∼ 105 particles for the disk. Gravitational forces of all the particles and their inelastic collisions are taken into account. Results. Dense short-wavelength wake structure is created by the disk self-gravity and a few global spiral arms are induced by the satellite. The self-gravity wakes regulate the orbital evolution of the satellite, which has been considered as a disk spreading mechanism, but not as a driver for the orbital evolution. Conclusions. The self-gravity wake torque to the satellite is so effective that the satellite migration is much faster than was predicted with the spiral arm torque. It provides a possible model to avoid the resonance capture of adjacent satellite pairs and establish the current orbital configuration of Saturn’s mid-sized satellites.

scholarly journals Departure from the Exact Location of Mean Motion Resonances Induced by the Gas Disk in Systems Observed by Kepler

2021 ◽  
Vol 161 (2) ◽  
pp. 77
Author(s):  
Su Wang ◽  
D. N. C. Lin ◽  
Xiaochen Zheng ◽  
Jianghui Ji
Keyword(s):  
Mean Motion Resonances ◽  
Exact Location ◽  
Mean Motion
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