scholarly journals Architectures of Exoplanetary Systems. III. Eccentricity and Mutual Inclination Distributions of AMD-stable Planetary Systems

2020 ◽  
Vol 160 (6) ◽  
pp. 276
Author(s):  
Matthias Y. He ◽  
Eric B. Ford ◽  
Darin Ragozzine ◽  
Daniel Carrera
Keyword(s):  
Planetary Systems ◽  
Exoplanetary Systems ◽  
Mutual Inclination

scholarly journals Stability analysis of three exoplanet systems

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.

scholarly journals Influence of the inclination damping on the formation of planetary systems

2014 ◽  
Vol 9 (S310) ◽  
pp. 220-222
Author(s):  
Sotiris Sotiriadis ◽  
Anne-Sophie Libert ◽  
Kleomenis Tsiganis
Keyword(s):  
Planetary Systems ◽  
Type Ii ◽  
Spin Orbit ◽  
Resonant Interactions ◽  
Extrasolar Systems ◽  
Mass Ratios ◽  
Mutual Inclination ◽  
Multiple Resonances ◽  
Hydrodynamical Simulations

AbstractHighly non-coplanar extrasolar systems (e.g. Upsilon Andromedae) and unexpected spin-orbit misalignment of some exoplanets have been discovered. In Libert and Tsiganis (2011), a significant increase of the mutual inclination of some multi-planet systems has been observed during the type II migration, as a result of planet-planet scattering and/or resonant interactions between the planets. Here we investigate the effect of the inclination damping due to planet-disk interactions on the previous results, for a variety of planetary systems with different initial configurations and mass ratios. Using the damping formulae for eccentricity and inclination provided by the numerical hydrodynamical simulations of Bitschet al.(2013), we examine their impact on the possible multiple resonances between the planets and how the growth in eccentricity and inclination is affected.

scholarly journals 1/1 resonant periodic orbits in three dimensional planetary systems

2014 ◽  
Vol 9 (S310) ◽  
pp. 82-83 ◽  
Author(s):  
Kyriaki I. Antoniadou ◽  
George Voyatzis ◽  
Harry Varvoglis
Keyword(s):  
Phase Space ◽  
Linear Stability ◽  
Periodic Orbits ◽  
Orbital Motion ◽  
Three Dimensional ◽  
Planetary Systems ◽  
Planetary Mass ◽  
Construct Maps ◽  
Mutual Inclination ◽  
Planar Family

AbstractWe study the dynamics of a two-planet system, which evolves being in a 1/1 mean motion resonance (co-orbital motion) with non-zero mutual inclination. In particular, we examine the existence of bifurcations of periodic orbits from the planar to the spatial case. We find that such bifurcations exist only for planetary mass ratios $\rho=\frac{m_2}{m_1}<0.0205$. For ρ in the interval 0<ρ<0.0205, we compute the generated families of spatial periodic orbits and their linear stability. These spatial families form bridges, which start and end at the same planar family. Along them the mutual planetary inclination varies. We construct maps of dynamical stability and show the existence of regions of regular orbits in phase space.

scholarly journals Planetary Systems

1999 ◽  
Vol 172 ◽  
pp. 313-316
Author(s):  
Pawel Artymowicz
Keyword(s):  
Radial Velocity ◽  
Main Sequence ◽  
Direct Evidence ◽  
Planetary System ◽  
Planetary Systems ◽  
Main Sequence Stars ◽  
The Past ◽  
Exoplanetary Systems ◽  
Beta Pictoris

AbstractThe past decade brought direct evidence of the previously surmised exoplanetary systems. A variety of planetary system types exist those around pulsars, around both young and old main-sequence stars (as evidenced by planetesimal disks of the Beta Pictoris-type), and the mature giant exoplanets found in radial velocity surveys. The surprising diversity of the exoplanetary systems is addressed by several theories of their origin.

scholarly journals Induced Kozai Migration and Formation of Close-in Planets in Binaries

2008 ◽  
Vol 4 (S253) ◽  
pp. 181-187
Author(s):  
Genya Takeda ◽  
Ryosuke Kita ◽  
Frederic A. Rasio
Keyword(s):  
Inclination Angle ◽  
Extrasolar Planets ◽  
Planetary Systems ◽  
Outer Planet ◽  
Momentum Exchange ◽  
Multiple Star ◽  
Tidal Friction ◽  
Orbital Decay ◽  
Planetary Orbits ◽  
Mutual Inclination

AbstractMany recent observational studies have concluded that planetary systems commonly exist in multiple-star systems. At least ~20%, and presumably a larger fraction, of the known extrasolar planetary systems are associated with one or more stellar companions. These stellar companions normally exist at large distances from the planetary systems (typical projected binary separations are 102–104AU) and are often faint (ranging from F to T spectral types). Yet, secular cyclic angular momentum exchange with these distant stellar companions can significantly alter the orbital configuration of the planets around the primaries. One of the most interesting and fairly common outcomes seen in numerical simulations is the opening of a large mutual inclination angle between the planetary orbits, forced by differential nodal precessions caused by the binary companion. The growth of the mutual inclination angle between planetary orbits induces additional large-amplitude eccentricity oscillations of the inner planet due to the quadrupole gravitational perturbation by the outer planet. This eccentricity oscillation may eventually result in the orbital decay of the inner planet through tidal friction, as previously proposed as Kozai migration or Kozai cycles with tidal friction (KCTF). This orbital decay mechanism induced by the binary perturbation and subsequent tidal dissipation may stand as an alternative formation channel for close-in extrasolar planets.

scholarly journals Understanding the assembly of Kepler's tightly-packed planetary systems

2014 ◽  
Vol 9 (S310) ◽  
pp. 90-92
Author(s):  
Thomas O. Hands ◽  
Richard D. Alexander ◽  
Walter Dehnen
Keyword(s):  
Initial Conditions ◽  
Planetary Systems ◽  
Dynamical Study ◽  
Exoplanetary Systems ◽  
Kepler Mission ◽  
And Migration

AbstractThe Kepler mission has recently discovered a number of exoplanetary systems, such as Kepler 11, in which ensembles of several planets are found in very closely packed orbits. These systems present a challenge for traditional formation and migration scenarios. We present a dynamical study of the evolution of these systems using an N-body approach, incorporating both smooth and stochastic migration forces and a variety of initial conditions, in order to assess the feasibility of assembling such systems via traditional, disc-driven migration.

scholarly journals Formation and Orbital Evolution of Planets

2011 ◽  
Vol 7 (S282) ◽  
pp. 429-436
Author(s):  
Wilhelm Kley
Keyword(s):  
Solar System ◽  
Gravitational Instability ◽  
Planetary Systems ◽  
Large Mass ◽  
Orbital Evolution ◽  
Protoplanetary Disk ◽  
Dynamical Structure ◽  
High Eccentricity ◽  
Exoplanetary Systems ◽  
Alternative Processes

AbstractThe formation of planetary systems is a natural byproduct of the star formation process. Planets can form inside the protoplanetary disk by two alternative processes. Either through a sequence of sticking collisions, the so-called sequential accretion scenario, or via gravitational instability from an over-dense clump inside the protoplanetary disk. The first process is believed to have occurred in the solar system. The most important steps in this process will be outlined. The observed orbital properties of exoplanetary systems are distinctly different from our own Solar System. In particular, their small distance from the star, their high eccentricity and large mass point to the existence of a phase with strong mutual excitations. These are believed to be a result of early evolution of planets due to planet-disk interaction. The importance of this process in shaping the dynamical structure of planetary systems will be presented.

scholarly journals EQUATIONS OF PLANETARY SYSTEMS MOTION

2020 ◽  
Vol 6 (334) ◽  
pp. 53-60
Author(s):  
M. Zh. Minglibayev ◽  
◽  
A.B. Kosherbayeva ◽  
Keyword(s):  
Main Part ◽  
Planetary Systems ◽  
Orbital Plane ◽  
Canonical System ◽  
Dynamic Evolution ◽  
Secular Perturbations ◽  
Exoplanetary Systems ◽  
Absolute Coordinates ◽  
The Masses ◽  
Exoplanet Systems

The study of the dynamically evolution of planetary systems is very actually in relation with findings of exoplanet systems. free spherical bodies problem is considered in this paper, mutually gravitating according to Newton's law, with isotropically variable masses as a celestial-mechanical model of non-stationary exoplanetary systems. The dynamic evolution of planetary systems is learned, when evolution's leading factor is the masses' variability of gravitating bodies themselves. The laws of the bodies' masses varying are assumed to be known arbitrary functions of time. When doing so the rate of varying of bodies' masses is different. The planets' location is such that the orbits of planets don't intersect. Let us treat this position of planets is preserve in the evolution course. The motions are researched in the relative coordinates system with beginning in the center of the parent star, axes that are parallel to corresponding axes of the absolute coordinates system. The canonical perturbation theory is used on the base aperiodic motion over the quasi-canonical cross-section. The bodies evolution is studied in the osculating analogues of the second system of canonical Poincare elements. The canonical equations of perturbed motion in analogues of the second system of canonical Poincare elements are convenient for describing the planetary systems dynamic evolution, when analogues of eccentricities and analogues of inclinations of orbital plane are sufficiently small. It is noted that to obtain an analytical expression of the perturbing function main part through canonical osculating Poincare elements using computer algebra is preferably. If in expansions of the main part of perturbing function is constrained with precision to second orders including relatively small quantities, then the equations of secular perturbations will obtained as linear non-autonomous system. This circumstance meaningful makes much easier to study the non-autonomous canonical system of differential equations of secular perturbations of considering problem.

scholarly journals Orbital eccentricity–multiplicity correlation for planetary systems and comparison to the Solar system

2020 ◽  
Vol 500 (1) ◽  
pp. 1313-1322
Author(s):  
Nanna Bach-Møller ◽  
Uffe G Jørgensen
Keyword(s):  
Solar System ◽  
Power Law ◽  
Planetary System ◽  
Planetary Systems ◽  
Detection Methods ◽  
Orbital Eccentricity ◽  
Full Data ◽  
Exoplanetary Systems ◽  
The One ◽  
Good Agreement

ABSTRACT The orbit eccentricities of the Solar system planets are unusually low compared to the average of known exoplanetary systems. A power-law correlation has previously been found between the multiplicity of a planetary system and the orbital eccentricities of its components, for systems with multiplicities above two. In this study we investigate the correlation for an expanded data sample by focusing on planetary systems as units (unlike previous studies that have focused on individual planets). Our full data sample contains 1171 exoplanets, in 895 systems, and the correlation between eccentricity and multiplicity is found to follow a clear power law for all multiplicities above one. We discuss the correlation for several individual subsamples and find that all samples consistently follow the same basic trend regardless of e.g. planet types and detection methods. We find that the eccentricities of the Solar system fit the general trend and suggest that the Solar system might not show uncommonly low eccentricities (as often speculated) but rather uncommonly many planets compared to a ‘standard’ planetary system. The only outlier from the power-law correlation is, consistently in all the samples, the one-planet systems. It has previously been suggested that this may be due to additional unseen exoplanets in the observed one-planet systems. Based on this assumption and the power-law correlation, we estimate that the probability of a system having eight planets or more is of the order of 1 per cent, in good agreement with recent predictions from analyses based on independent arguments.

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