Chaotic Orbits Within the 3-2 Jovian Mean Motion Resonance

1995 ◽  
Vol 110 ◽  
pp. 1879
Author(s):  
Fred A. Franklin
Keyword(s):  
Mean Motion ◽  
Chaotic Orbits ◽  
Mean Motion Resonance

scholarly journals On a possibility of transfer of asteroids from the 2:1 mean motion resonance with Jupiter to the Centaur zone

2021 ◽  
Author(s):  
Kazantsev Anatolii ◽  
Kazantseva Lilia
Keyword(s):  
Terrestrial Planet ◽  
Numerical Calculations ◽  
Asteroid Belt ◽  
Time Interval ◽  
Transfer Time ◽  
Mean Motion ◽  
Resonant Orbits ◽  
Main Asteroid Belt ◽  
Absolute Magnitudes ◽  
Mean Motion Resonance

ABSTRACT The paper analyses possible transfers of bodies from the main asteroid belt (MBA) to the Centaur region. The orbits of asteroids in the 2:1 mean motion resonance (MMR) with Jupiter are analysed. We selected the asteroids that are in resonant orbits with e > 0.3 whose absolute magnitudes H do not exceed 16 m. The total number of the orbits amounts to 152. Numerical calculations were performed to evaluate the evolution of the orbits over 100,000-year time interval with projects for the future. Six bodies are found to have moved from the 2:1 commensurability zone to the Centaur population. The transfer time of these bodies to the Centaur zone ranges from 4,600 to 70,000 yr. Such transfers occur after orbits leave the resonance and the bodies approach Jupiter Where after reaching sufficient orbital eccentricities bodies approach a terrestrial planet, their orbits go out of the MMR. Accuracy estimations are carried out to confirm the possible asteroid transfers to the Centaur region.

scholarly journals New Constraints on Gliese 876—Exemplar of Mean-motion Resonance

2018 ◽  
Vol 155 (3) ◽  
pp. 106 ◽  
Author(s):  
Sarah Millholland ◽  
Gregory Laughlin ◽  
Johanna Teske ◽  
R. Paul Butler ◽  
Jennifer Burt ◽  
...  
Keyword(s):  
Mean Motion ◽  
Mean Motion Resonance

scholarly journals On the Super-Earths locked in the 3:2 mean-motion resonance

2010 ◽  
Vol 42 ◽  
pp. 287-290
Author(s):  
A. Łacny ◽  
E. Szuszkiewicz
Keyword(s):  
Mean Motion ◽  
Mean Motion Resonance

scholarly journals Analysis of near-separatrix motion in planetary systems

2007 ◽  
Vol 3 (S249) ◽  
pp. 491-498
Author(s):  
Su Wang ◽  
Ji-Lin Zhou
Keyword(s):  
Planetary Systems ◽  
Scattering Model ◽  
High Occurrence ◽  
Mean Motion ◽  
Accretion Process ◽  
Three Body ◽  
Mean Motion Resonance

AbstractNear-separatrix motion is a kind of motion of two planets with their relative apsidal longitude near the boundary between libration and circulation. Observed multiple planetary systems seem to favor near-separatrix motions between neighboring planets. In this report, we study the probability that near-separatrix motion occurs with both the linear secular system and full three-body systems. We find that generally the ratio of near-separatrix motion is small unless the eccentricities of the two planets differ from each other by an order of magintude, or they are in mean motion resonance. To explore the dynamical procedures causing the near-separatrix motion, we suppose a modification to scattering model by adding a mass-accretion process during the protoplanet growth. Statistics on the modified scattering model indicate that the probability of the final planet pairs in near-separatrix motion is high (∼ 85%), which may explain the high occurrence of near-separatrix motions in observed planetary systems.

scholarly journals Horseshoe co-orbitals of Earth: current population and new candidates

2020 ◽  
Vol 496 (4) ◽  
pp. 4420-4432
Author(s):  
Murat Kaplan ◽  
Sergen Cengiz
Keyword(s):  
Solar System ◽  
Semimajor Axis ◽  
Dynamical Behaviour ◽  
Orbital State ◽  
Mean Motion ◽  
Current Population ◽  
Mean Motion Resonance

ABSTRACT Most co-orbital objects in the Solar system are thought to follow tadpole-type orbits, behaving as Trojans. However, most of Earth’s identified co-orbitals are moving along horseshoe-type orbits. The current tally of minor bodies considered to be Earth co-orbitals amounts to 18; of them, 12 are horseshoes, 5 are quasi-satellites, and 1 is a Trojan. The semimajor axis values of all these bodies librate between 0.983 and 1.017 au. In this work, we have studied the dynamical behaviour of objects following orbits with semimajor axis within this range that may be in a 1:1 mean-motion resonance with Earth. Our results show that asteroids 2016 CO246, 2017 SL16, and 2017 XQ60 are moving along asymmetrical horseshoe-type orbits; the asteroid 2018 PN22 follows a nearly symmetric or regular horseshoe-type orbit. Asteroids 2016 CO246, 2017 SL16, and 2017 XQ60 can remain in the horseshoe co-orbital state for about 900, 3300, and 2700 yr, respectively. Asteroid 2018 PN22 has a more chaotic dynamical behaviour; it may not stay in a horseshoe co-orbital state for more than 200 yr. The horseshoe libration periods of 2016 CO246, 2017 SL16, 2017 XQ60, and 2018 PN22 are 280, 255, 411, and 125 yr, respectively.

scholarly journals A resonant pair of warm giant planets revealed by TESS

2019 ◽  
Vol 486 (4) ◽  
pp. 4980-4986 ◽  
Author(s):  
David Kipping ◽  
David Nesvorný ◽  
Joel Hartman ◽  
Guillermo Torres ◽  
Gaspar Bakos ◽  
...  
Keyword(s):  
Giant Planets ◽  
Dynamical Model ◽  
First Year ◽  
Mean Motion ◽  
M Dwarf ◽  
Mean Motion Resonance ◽  
Dynamical Masses

ABSTRACT We present the discovery of a pair of transiting giant planets using four sectors of TESS photometry. TOI-216 is a 0.87 M⊙ dwarf orbited by two transiters with radii of 8.2 and 11.3 R⊕, and periods of 17.01 and 34.57 d, respectively. Anticorrelated TTVs are clearly evident indicating that the transiters orbit the same star and interact via a near 2:1 mean motion resonance. By fitting the TTVs with a dynamical model, we infer masses of $30_{-14}^{+20}$ and $200_{-100}^{+170}$ M⊕, establishing that the objects are planetary in nature and have likely sub-Kronian and Kronian densities. TOI-216 lies close to the southern ecliptic pole and thus will be observed by TESS throughout the first year, providing an opportunity for continuous dynamical monitoring and considerable refinement of the dynamical masses presented here. TOI-216 closely resembles Kepler-9 in architecture, and we hypothesize that in such systems these Saturn analogues failed to fully open a gap and thus migrated far deeper into the system before becoming trapped into resonance, which would imply that future detections of new analogues may also have sub-Jupiter masses.

scholarly journals Impactor Flux on the Pluto-Charon System

2009 ◽  
Vol 5 (S263) ◽  
pp. 98-101 ◽  
Author(s):  
Gonzalo C. de Elía ◽  
Romina P. Di Sisto ◽  
Adrián Brunini
Keyword(s):  
Size Distribution ◽  
Kuiper Belt ◽  
Primary Source ◽  
Mean Motion ◽  
Stability And Instability ◽  
The Stability ◽  
Mean Motion Resonance ◽  
Collisional Evolution

AbstractIn this work, we study the impactor flux on Pluto and Charon due to the collisional evolution of Plutinos.To do this, we develop a statistical code that includes catastrophic collisions and cratering events, and takes into account the stability and instability zones of the 3:2 mean motion resonance with Neptune. Our results suggest that if 1 Pluto-sized object is in this resonance, the flux of D = 2 km Plutinos on Pluto is ~4–24 percent of the flux of D = 2 km Kuiper Belt projectiles on Pluto. However, with 5 Pluto-sized objects in the resonance, the contribution of the Plutino population to the impactor flux on Pluto may be comparable to that of the Kuiper Belt. As for Charon, if 1 Pluto-sized object is in the 3:2 resonance, the flux of D = 2 km Plutinos is ~10–63 percent of the flux of D = 2 km impactors coming from the Kuiper Belt. However, with 5 Pluto-sized objects, the Plutino population may be a primary source of the impactor flux on Charon. We conclude that it is necessary to specify the Plutino size distribution and the number of Pluto-sized objects in the 3:2 Neptune resonance in order to determine if the Plutino population is a primary source of impactors on the Pluto-Charon system.

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