On the Stability of the Terrestrial Planets as Models for Exosolar Planetary Systems

In this chapter, the author summarizes the properties of the Solar System, and how these were uncovered. Over centuries, the arrangement and properties of the Solar System were determined. The distinctions between the terrestrial planets, the gas and ice giants, and their various moons are discussed. Whereas humans have walked only on the Moon, probes have visited all the planets and several moons, asteroids, and comets; samples have been returned to Earth only from our moon, a comet, and from interplanetary dust. For Earth and Moon, seismographs probed their interior, whereas for other planets insights come from spacecraft and meteorites. We learned that elements separated between planet cores and mantels because larger bodies in the Solar System were once liquid, and many still are. How water ended up where it is presents a complex puzzle. Will the characteristics of our Solar System hold true for planetary systems in general?

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Retrograde resonances in compact multi-planetary systems: a feasible stabilizing mechanism

Proceedings of the International Astronomical Union ◽

10.1017/s1743921308017055 ◽

2007 ◽

Vol 3 (S249) ◽

pp. 511-516 ◽

Cited By ~ 1

Author(s):

Julie Gayon ◽

Eric Bois

Keyword(s):

Body Problem ◽

Extrasolar Planets ◽

Planetary Systems ◽

Central Star ◽

Point Of View ◽

Outer Planet ◽

Mean Motion Resonances ◽

Hot Jupiters ◽

The Stability ◽

Orbital Data

AbstractMulti-planet systems detected until now are in most cases characterized by hot-Jupiters close to their central star as well as high eccentricities. As a consequence, from a dynamical point of view, compact multi-planetary systems form a variety of the general N-body problem (with N ≥ 3), whose solutions are not necessarily known. Extrasolar planets are up to now found in prograde (i.e. direct) orbital motions about their host star and often in mean-motion resonances (MMR). In the present paper, we investigate a theoretical alternative suitable for the stability of compact multi-planetary systems. When the outer planet moves on a retrograde orbit in MMR with respect to the inner planet, we find that the so-called retrograde resonances present fine and characteristic structures particularly relevant for dynamical stability. We show that retrograde resonances and their resources open a family of stabilizing mechanisms involving specific behaviors of apsidal precessions. We also point up that for particular orbital data, retrograde MMRs may provide more robust stability compared to the corresponding prograde MMRs.

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Post‐oligarchic Evolution of Protoplanetary Embryos and the Stability of Planetary Systems

The Astrophysical Journal ◽

10.1086/519918 ◽

2007 ◽

Vol 666 (1) ◽

pp. 423-435 ◽

Cited By ~ 103

Author(s):

Ji‐Lin Zhou ◽

Douglas N. C. Lin ◽

Yi‐Sui Sun

Keyword(s):

Planetary Systems ◽

The Stability

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The Stability of Planetary Systems

10.1007/978-94-009-5331-4 ◽

1985 ◽

Keyword(s):

Planetary Systems ◽

The Stability

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Stability analysis of three exoplanet systems

Monthly Notices of the Royal Astronomical Society ◽

10.1093/mnras/staa847 ◽

2020 ◽

Vol 494 (2) ◽

pp. 2280-2288

Author(s):

J P Marshall ◽

J Horner ◽

R A Wittenmyer ◽

J T Clark ◽

M W Mengel

Keyword(s):

Time Scales ◽

Planetary Systems ◽

Orbital Parameters ◽

Exoplanetary Systems ◽

Best Fitting ◽

The Stability ◽

Short Time ◽

Exoplanet Systems ◽

Best Fit

ABSTRACT The orbital solutions of published multiplanet systems are not necessarily dynamically stable on time-scales comparable to the lifetime of the system as a whole. For this reason, dynamical tests of the architectures of proposed exoplanetary systems are a critical tool to probe the stability and feasibility of the candidate planetary systems, with the potential to point the way towards refined orbital parameters of those planets. Such studies can even help in the identification of additional companions in such systems. Here, we examine the dynamical stability of three planetary systems, orbiting HD 67087, HD 110014, and HD 133131A. We use the published radial velocity measurements of the target stars to determine the best-fitting orbital solutions for these planetary systems using the systemic console. We then employ the N-body integrator mercury to test the stability of a range of orbital solutions lying within 3σ of the nominal best fit for a duration of 100 Myr. From the results of the N-body integrations, we infer the best-fitting orbital parameters using the Bayesian package astroemperor. We find that both HD 110014 and HD 133131A have long-term stable architectures that lie within the 1σ uncertainties of the nominal best fit to their previously determined orbital solutions. However, the HD 67087 system exhibits a strong tendency towards instability on short time-scales. We compare these results to the predictions made from consideration of the angular momentum deficit criterion, and find that its predictions are consistent with our findings.

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Formation of Habitable Planets in Inclined Planetary Systems

Proceedings of the International Astronomical Union ◽

10.1017/s1743921313012908 ◽

2012 ◽

Vol 8 (S293) ◽

pp. 238-240

Author(s):

Jianghui Ji ◽

Sheng Jin

Keyword(s):

Late Stage ◽

Planetary Systems ◽

Numerical Results ◽

The Other ◽

Terrestrial Planets ◽

Habitable Zone ◽

Planetary Formation ◽

Habitable Planets ◽

Final Assembly ◽

Inner Region

AbstractWe extensively investigate the terrestrial planetary formation for the inclined planetary systems (considering the OGLE-2006-BLG-109L system as example) in the late stage. In the simulations, we show that the occurrence of terrestrial planets appears to be common in the final assembly stage. Moreover, we find that a lot of runs finally occupy at least one planet in the habitable zone (HZ). On the other hand, the numerical results also indicate that the inner region of the planetesimal disk, ranging from ~ 0.1 to 0.3 AU, plays an important role in building up terrestrial planets. The outcomes suggest that it may exist moderate possibility for the inclined systems to harbor terrestrial planets in the HZ.

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