Numerical simulations of the accretion of Uranus and Neptune. II. Effect of low velocity encounters

1999 ◽  
Vol 173 ◽  
pp. 31-36 ◽  
Author(s):  
A. Brunini ◽  
J.A. Fernández
Keyword(s):  
Solar System ◽  
Numerical Simulations ◽  
Numerical Experiments ◽  
Relative Velocity ◽  
Solid Material ◽  
Outer Solar System ◽  
Low Velocity ◽  
Mean Motion Resonances ◽  
Outer Planets ◽  
Accretion Process

AbstractNew numerical simulations of the accretion of the outer solar system were carried out by means of a symplectic integration code developed by the authors. By contrast with our previous numerical experiments, we now pay special attention to the treatment of low relative velocity encounters between planetesimals. Our new results corroborate, in general, a marked radial drift of the accreting outer planets, and that less than 50% of the solid material originally present in the system contributes to the accretion process. The results confirm that mean motion resonances play a major role during the accretion of the outer solar system.

scholarly journals Low Velocity Encounters of Minor Bodies With the Outer Planets

1983 ◽  
Vol 74 ◽  
pp. 377-395
Author(s):  
A. Carusi ◽  
E. Perozzi ◽  
G.B. Valsecchi
Keyword(s):  
Solar System ◽  
Orbital Evolution ◽  
Outer Solar System ◽  
Low Velocity ◽  
Minor Body ◽  
Outer Planets ◽  
Close Encounters ◽  
Satellite Capture

Previous studies of close encounters of minor bodies with Jupiter have shown that the perturbations are stronger either if the encounter is very deep or if the velocity of the minor body relative to the planet is low. In the present research we investigate the effects of low velocity encounters between fictitious minor bodies and the four outer planets. Two possible outcomes of this type of encounter are the temporary satellite capture of the minor body by the planet, and the exchange of perihelion with aphelion of the minor body orbit. Different occurrence rates of these processes are found for different planets, and the implications for the orbital evolution of minor bodies in the outer Solar System are discussed.

scholarly journals Numerical Experiments on the Motion of the Outer Planets

1992 ◽  
Vol 152 ◽  
pp. 25-32 ◽  
Author(s):  
Gerald D. Quinlan
Keyword(s):  
Lyapunov Exponent ◽  
Solar System ◽  
Probability Distribution ◽  
Numerical Experiments ◽  
Initial Conditions ◽  
Major Axis ◽  
Solar Systems ◽  
Outer Planets ◽  
System A ◽  
Real Value

We have integrated the motion of the four Jovian planets on Myr timescales in fictitious solar systems in which the orbits differ from those of the real solar system. A change of ≲1% in the major axis of any one of the planets from its real value can lead to chaotic motion with a Lyapunov exponent larger than 10-5 yr−1. A survey of fifty solar systems with initial conditions chosen at random from a reasonable probability distribution shows the majority of them to be chaotic.

scholarly journals A scattered Uranus and Neptune, and implications for the asteroid belt

2004 ◽  
Vol 202 ◽  
pp. 241-243
Author(s):  
Edward W. Thommes ◽  
Martin J. Duncan ◽  
Harold F. Levison ◽  
John E. Chambers
Keyword(s):  
Solar System ◽  
Numerical Simulations ◽  
Initial Conditions ◽  
Asteroid Belt ◽  
Outer Solar System ◽  
Wide Range ◽  
Gas Giant ◽  
Gas Accretion ◽  
High Degree

It has been proposed that Uranus and Neptune originated interior to ∽ 10 AU, as potential gas giant cores which were scattered outward when Jupiter won the race to reach runaway gas accretion. We present further numerical simulations of this scenario, which show that it reproduces the present configuration of the outer Solar System with a high degree of success for a wide range of initial conditions. Also, we show that this mechanism may have simultaneously ejected planets from the asteroid belt.

The contribution of Centaur-emitted dust to the interplanetary dust distribution

2019 ◽  
Vol 490 (2) ◽  
pp. 2421-2429 ◽  
Author(s):  
A R Poppe
Keyword(s):  
Solar System ◽  
Mass Loss ◽  
Kuiper Belt ◽  
Interplanetary Dust ◽  
Outer Solar System ◽  
Dust Grains ◽  
Kuiper Belt Objects ◽  
Dust Density ◽  
Outer Planets ◽  
Current Mass

ABSTRACT Interplanetary dust grains originate from a variety of source bodies, including comets, asteroids, and Edgeworth–Kuiper belt objects. Centaurs, generally defined as those objects with orbits that cross the outer planets, have occasionally been observed to exhibit cometary-like outgassing at distances beyond Jupiter, implying that they may be an important source of dust grains in the outer Solar system. Here, we use an interplanetary dust grain dynamics model to study the behaviour and equilibrium distribution of Centaur-emitted interplanetary dust grains. We focus on the five Centaurs with the highest current mass-loss rates: 29P/Schwassmann-Wachmann 1, 166P/2001 T4, 174P/Echeclus, C/2001 M10, and P/2004 A1, which together comprise 98 per cent of the current mass loss from all Centaurs. Our simulations show that Centaur-emitted dust grains with radii s < 2 μm have median lifetimes consistent with Poynting–Robertson (P–R) drag lifetimes, while grains with radii s > 2 μm have median lifetimes much shorter than their P–R drag lifetimes, suggesting that dynamical interactions with the outer planets are effective in scattering larger grains, in analogy to the relatively short lifetimes of Centaurs themselves. Equilibrium density distributions of grains emitted from specific Centaurs show a variety of structure including local maxima in the outer Solar system and azimuthal asymmetries, depending on the orbital elements of the parent Centaur. Finally, we compare the total Centaur interplanetary dust density to dust produced from Edgeworth–Kuiper belt objects, Jupiter-family comets, and Oort cloud comets, and conclude that Centaur-emitted dust may be an important component between 5 and 15 au, contributing approximately 25 per cent of the local interplanetary dust density at Saturn.

scholarly journals Long Term Evolution of the Solar System

1992 ◽  
Vol 152 ◽  
pp. 17-24 ◽  
Author(s):  
Jack Wisdom
Keyword(s):  
Solar System ◽  
Test Particle ◽  
Long Term Evolution ◽  
Mapping Method ◽  
Outer Solar System ◽  
Central Mass ◽  
Outer Planets ◽  
Term Evolution ◽  
Particle Stability

The mapping method of Wisdom (1982) has been generalized to encompass all n-body problems with a dominant central mass (Wisdom and Holman, 1991). The new mapping method is presented as well as a number of initial applications. These include billion year integrations of the outer planets, a number of 100 million year integrations of the whole solar system, and a systematic survey of test particle stability in the outer solar system.

Prebiotic-Related Chemistry in the Present Outer Solar System

1997 ◽  
Vol 161 ◽  
pp. 401-412
Author(s):  
François Raulin ◽  
Patrice Coll ◽  
Marie-Claire Gazeau ◽  
Paul Bruston
Keyword(s):  
Solar System ◽  
Liquid Water ◽  
Prebiotic Chemistry ◽  
Outer Solar System ◽  
Outer Planets ◽  
Organic Systems ◽  
Long Time ◽  
Planetary Environment ◽  
Complex Organic ◽  
Natural Laboratory

AbstractThere are numerous places in the outer solar system where the formation of the starting ingredients which are involved in the early terrestrial prebiotic chemistry is currently going on. Organic chemistry is largely present in the outer planets, particularly in Titan. Titan has a dense atmosphere, mainly composed of N2and CH4and very rich in organic compounds, both in gas and aerosol phases. Because of the low temperature of Titan’s environment, liquid water is currently absent from the satellite and compounds of low stability at the (Earth) laboratory temperature, and very reactive, are still or may be present. However, Titan study should provide information on prebiotic chemistry – at least prebiotic chemistry in absence of liquid water. This quasi-planet thus appears as a natural laboratory enabling to study prebiotic evolution toward complex organic systems in a planetary environment over a long time scale. A detailed study of such a natural prebiotic laboratory is precisely one of the main objectives of the Cassini-Huygens mission. With the sending of the Cassini orbiter around Saturn and the Huygens probe in the atmosphere of Titan, this mission, due to be launched in October 1997, for a Saturn arrival in 2004, will offer a unique opportunity to study in detail extra-terrestrial prebiotic processes, together with important implications in the field of bioastronomy and the origins of life.

scholarly journals Transit of asteroids across the 7/3 Kirkwood gap under the Yarkovsky effect

2020 ◽  
Vol 637 ◽  
pp. A19
Author(s):  
Yang-Bo Xu ◽  
Li-Yong Zhou ◽  
Wing-Huen Ip
Keyword(s):  
Solar System ◽  
Numerical Simulations ◽  
Observational Data ◽  
Family Members ◽  
Main Belt ◽  
Mean Motion Resonances ◽  
Yarkovsky Effect ◽  
Principal Source ◽  
Kirkwood Gap ◽  
Near Earth Objects

The Yarkovsky effect plays an important role in asteroids drifting in the inner Solar System. In the main belt, many asteroids are continuously pushed by the Yarkovsky effect into regions of different mean motion resonances (MMRs) and then ejected after a period of time, due to the instability of MMRs. They are considered as the principal source of near-Earth objects. In this paper, we investigate the effects of the 7/3 MMR with Jupiter (J7/3 MMR) on the transportation of asteroids from the Koronis family and the Eos family that reside, respectively, on the inner and outer sides of the resonance using numerical simulations. The J7/3 MMR acts like a selective barrier to migrating asteroids. The fraction of asteroids that successfully cross through the resonance and the escape rate from the resonance are found to depend on the Yarkovsky drifting rate, the initial inclination and the migrating direction. The excitation of eccentricity and inclination due to the combined influence from both the resonance and the Yarkovsky effect are discussed. Only the eccentricity can be pumped up considerably, and it is attributed mainly to the resonance. In the observational data, family members are also found in the resonance and on the opposite side of the resonance with respect to the corresponding family centre. The existence of these family members is explained using our results of numerical simulations. Finally, the replenishment of asteroids in the J7/3 MMR and its transportation of asteroids are discussed.

scholarly journals Carlsberg optical astrometry of the outer solar system

1996 ◽  
Vol 172 ◽  
pp. 399-406
Author(s):  
L.V. Morrison ◽  
M.E. Buontempo
Keyword(s):  
Solar System ◽  
Optical Observations ◽  
Outer Solar System ◽  
Outer Planets ◽  
Run Off ◽  
Solar System Objects

The Carlsberg astrometric telescope has made about 17000 observations of outer Solar System objects since it began operation in 1984. The observed positions of the major planets are compared with JPL DE200 and DE403. The agreement with DE403 is good in general, but unresolved discrepancies of the order 0″.1 are found in Jupiter and Saturn. The run-off between the observations and DE200 which was fitted to observations before 1980 emphasize the need to continue optical observations of the outer planets.

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