scholarly journals Capture and migration of Jupiter and Saturn in mean motion resonance in a gaseous protoplanetary disc

2020 ◽  
Vol 492 (4) ◽  
pp. 6007-6018 ◽  
Author(s):  
Raúl O Chametla ◽  
Gennaro D’Angelo ◽  
Mauricio Reyes-Ruiz ◽  
F Javier Sánchez-Salcedo
Keyword(s):  
Solar Nebula ◽  
Dynamical Evolution ◽  
Giant Planets ◽  
Orbital Dynamics ◽  
Evolutionary Path ◽  
Mean Motion ◽  
Evolutionary Scenario ◽  
Low Probability ◽  
And Migration ◽  
Mean Motion Resonance

ABSTRACT We study the dynamical evolution of Jupiter and Saturn embedded in a gaseous, solar nebula-type disc by means of hydrodynamics simulations with the fargo2d1d code. We study the evolution for different initial separations of the planets’ orbits, ΔaSJ, to investigate whether they become captured in mean motion resonance (MMR) and the direction of the subsequent migration of the planet (inwards or outwards). We also provide an assessment of the planet’s orbital dynamics at different epochs of Saturn’s growth. We find that the evolution of initially compact orbital configurations is dependent on the value of ΔaSJ. This implies that an evolution as that proposed in the Grand Tack model depends on the precise initial orbits of Jupiter and Saturn and on the time-scales for their formation. Capture in the 1:2 MMR and inward or (nearly) stalled migration are highly favoured. Within its limits, our work suggests that the reversed migration, associated with the resonance capture of Jupiter and Saturn, may be a low-probability evolutionary scenario, so that other planetary systems with giant planets are not expected to have experienced a Grand Tack-like evolutionary path.

scholarly journals A Pair of Warm Giant Planets near the 2:1 Mean Motion Resonance around the K-dwarf Star TOI-2202*

2021 ◽  
Vol 162 (6) ◽  
pp. 283
Author(s):  
Trifon Trifonov ◽  
Rafael Brahm ◽  
Nestor Espinoza ◽  
Thomas Henning ◽  
Andrés Jordán ◽  
...  
Keyword(s):  
Orbital Period ◽  
Dynamical Evolution ◽  
Giant Planets ◽  
Light Curves ◽  
Dynamical Analysis ◽  
Dwarf Star ◽  
Mean Motion ◽  
Robotic Telescope ◽  
Mean Motion Resonance

Abstract TOI-2202 b is a transiting warm Jovian-mass planet with an orbital period of P = 11.91 days identified from the Full Frame Images data of five different sectors of the TESS mission. Ten TESS transits of TOI-2202 b combined with three follow-up light curves obtained with the CHAT robotic telescope show strong transit timing variations (TTVs) with an amplitude of about 1.2 hr. Radial velocity follow-up with FEROS, HARPS, and PFS confirms the planetary nature of the transiting candidate (a b = 0.096 ± 0.001 au, m b = 0.98 ± 0.06 M Jup), and a dynamical analysis of RVs, transit data, and TTVs points to an outer Saturn-mass companion (a c = 0.155 ± 0.002 au, m c = 0.37 ± 0.10 M Jup) near the 2:1 mean motion resonance. Our stellar modeling indicates that TOI-2202 is an early K-type star with a mass of 0.82 M ⊙, a radius of 0.79 R ⊙, and solar-like metallicity. The TOI-2202 system is very interesting because of the two warm Jovian-mass planets near the 2:1 mean motion resonance, which is a rare configuration, and their formation and dynamical evolution are still not well understood.

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 What to Expect from Transiting Multiplanet Systems

2008 ◽  
Vol 4 (S253) ◽  
pp. 173-179 ◽  
Author(s):  
Daniel C. Fabrycky
Keyword(s):  
Radial Velocity ◽  
Transit Time ◽  
Dynamical Evolution ◽  
Velocity Measurements ◽  
Search Methods ◽  
Tidal Evolution ◽  
Transiting Planets ◽  
Mean Motion ◽  
Time Variations ◽  
Mean Motion Resonance

AbstractSo far radial velocity measurements have discovered ~25 stars to host multiple planets. The statistics imply that many of the known hosts of transiting planets should have additional planets, yet none have been solidly detected. They will be soon, via complementary search methods of RV, transit-time variations of the known planet, and transits of the additional planet. When they are found, what can transit measurements add to studies of multiplanet dynamical evolution? First, mutual inclinations become measurable, for comparison to the solar system's disk-like configuration. Such measurements will give important constraints to planet-planet scattering models, just as the radial velocity measurements of eccentricity have done. Second, the Rossiter-McLaughlin effect measures stellar obliquity, which can be modified by two-planet dynamics with a tidally evolving inner planet. Third, transit-time variations are exquisitely sensitive to planets in mean motion resonance. Two planets differentially migrating in the disk can establish such resonances, and tidal evolution of the planets can break them, so the configuration and frequency of these resonances as a function of planetary parameters will constrain these processes.

scholarly journals Formation and transformation of the 3:1 mean-motion resonance in 55 Cancri System

2007 ◽  
Vol 3 (S249) ◽  
pp. 485-490 ◽  
Author(s):  
Li-Yong Zhou ◽  
Sylvio Ferraz-Mello ◽  
Yi-Sui Sun
Keyword(s):  
Configuration Space ◽  
Rate Increase ◽  
Dynamical Evolution ◽  
Resonance Capture ◽  
Resonance System ◽  
Mean Motion ◽  
Damping Rate ◽  
Orbital Configuration ◽  
Planetary Migration ◽  
Mean Motion Resonance

AbstractWe report in this paper the numerical simulations of the capture into the 3:1 mean-motion resonance between the planets b and c in the 55 Cancri system. The results show that this resonance can be obtained by a differential planetary migration. The moderate initial eccentricities, relatively slower migration and suitable eccentricity damping rate increase significantly the probability of being trapped in this resonance. Otherwise, the system crosses the 3:1 commensurability avoiding resonance capture, to be eventually captured into a 2:1 resonance or some other higher-order resonances. After capture into resonance, the system can jump from one orbital configuration to another one if the migration continues, making a large region of the configuration space accessible for a resonance system. These investigations help us understand the diversity of resonance configurations and put some constraints on the early dynamical evolution of orbits in the extra-solar planetary systems.

The Influence of Giant Planets Near a Mean Motion Resonance on Earth‐like Planets in the Habitable Zone of Sun‐like Stars

2008 ◽  
Vol 681 (2) ◽  
pp. 1639-1645 ◽  
Author(s):  
E. Pilat‐Lohinger ◽  
Á. Süli ◽  
P. Robutel ◽  
F. Freistetter
Keyword(s):  
Giant Planets ◽  
Habitable Zone ◽  
Mean Motion ◽  
Earth Like Planets ◽  
Mean Motion Resonance

scholarly journals Long-term evolution of asteroids in the 2:1 Mean Motion Resonance

2014 ◽  
Vol 9 (S310) ◽  
pp. 178-179
Author(s):  
Despoina K. Skoulidou ◽  
Kleomenis Tsiganis ◽  
Harry Varvoglis
Keyword(s):  
Giant Planets ◽  
Dynamical Models ◽  
Mean Motion Resonances ◽  
First Order ◽  
Mean Motion ◽  
System A ◽  
Term Evolution ◽  
Approximate Treatment ◽  
Mean Motion Resonance

AbstractThe problem of the origin of asteroids residing in the Jovian first-order mean motion resonances is still open. Is the observed population survivors of a much larger population formed in the resonance in primordial times? Here, we study the evolution of 182 long-lived asteroids in the 2:1 Mean Motion Resonance, identified in Brož & Vokrouhlické (2008). We numerically integrate their trajectories in two different dynamical models of the solar system: (a) accounting for the gravitational effects of the four giant planets (i.e. 4-pl) and (b) adding the terrestrial planets from Venus to Mars (i.e. 7-pl). We also include an approximate treatment of the Yarkovksy effect (as in Tsiganis et al.2003), assuming appropriate values for the asteroid diameters.

scholarly journals Timing of the formation and migration of giant planets as constrained by CB chondrites

2016 ◽  
Vol 2 (12) ◽  
pp. e1601658 ◽  
Author(s):  
Brandon C. Johnson ◽  
Kevin J. Walsh ◽  
David A. Minton ◽  
Alexander N. Krot ◽  
Harold F. Levison
Keyword(s):  
Solar System ◽  
Solar Nebula ◽  
Giant Planet ◽  
Planetary Systems ◽  
Early Time ◽  
High Impact ◽  
Giant Planets ◽  
Significant Fraction ◽  
Carbonaceous Chondrites ◽  
And Migration

The presence, formation, and migration of giant planets fundamentally shape planetary systems. However, the timing of the formation and migration of giant planets in our solar system remains largely unconstrained. Simulating planetary accretion, we find that giant planet migration produces a relatively short-lived spike in impact velocities lasting ~0.5 My. These high-impact velocities are required to vaporize a significant fraction of Fe,Ni metal and silicates and produce the CB (Bencubbin-like) metal-rich carbonaceous chondrites, a unique class of meteorites that were created in an impact vapor-melt plume ~5 My after the first solar system solids. This indicates that the region where the CB chondrites formed was dynamically excited at this early time by the direct interference of the giant planets. Furthermore, this suggests that the formation of the giant planet cores was protracted and the solar nebula persisted until ~5 My.

scholarly journals Runaway migration in a multiple-protoplanet system

2007 ◽  
Vol 3 (S249) ◽  
pp. 413-418
Author(s):  
Hui Zhang ◽  
Ji-Lin Zhou
Keyword(s):  
Giant Planets ◽  
Stellar Disk ◽  
Wave Flow ◽  
Outer Planet ◽  
Mean Motion ◽  
The Mean ◽  
Orbital Region ◽  
Mean Motion Resonance

AbstractWe investigate the migration of two giant planets embedded in a proto-stellar disk. The inner planet(initially located at R10=1) is of 1 Jupiter mass and the outer one(R20=1.5) is of 1 Saturn mass. We find that due to the existence of the inner massive planet, the outer planet can not open a clear gap. Instead of an inward migration and being captured by the mean motion resonance of the inner planet, the outer planet undergoes an outward runaway migration. We conclude that this runaway migration is caused by the co-rotation torque in the co-orbital region of the outer planet and sustained by the wave(flow) driven by the inner massive planet.

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