Numerical modelling of Kuiper belt objects’ dynamics – limitations

1999 ◽  
Vol 173 ◽  
pp. 315-320
Author(s):  
R. Gabryszewski
Keyword(s):  
Solar System ◽  
Equations Of Motion ◽  
Kuiper Belt ◽  
Dynamical Evolution ◽  
Orbital Evolution ◽  
Time Span ◽  
Integration Time ◽  
Central Mass ◽  
Numerical Noise ◽  
Long Time

AbstractThe investigation of KBOs’ dynamics is based on numerical orbital integrations on extremly long time scales due to orbital evolution of particles. The evolution of KBOs to JFCs needs a time-span of order of 109years. Such a long time of integration affects errors. So the question arises what is the boundary of an integration time to distinguish the physical solution from numerical noise and what it depends on. This paper presents numerical integrations of less than 150 massless test particles in the model of the Solar System which consists of 4 giant planets and the central mass. For each test particle computations were repeated at least twice on different computers and using two different methods of integration. The results show that an increase of errors in a solution depends on the eccentricity and the inclination of an orbit. The estimated maximum time-span of integration is of the order of 10 million years for highly elliptic orbits (e 0.6) and up to 125 million years for quasi-circular orbits (for particular model of the Solar System with orbits of massless objects outside Neptune's orbit). After long time-span of integration (120-130 Myrs) the solution can be completely chaotic. It cannot be stated unequivocally that this is one of the possible particle's paths or that this is just a numerical noise. So a different way of studying KBOs’ and SP comets’ dynamical evolution is needed. The integration of equations of motion between particular phases of objects which are considered as comets in different phases of their lives (KBOs − Centaurs − Comets − possibly extinct Comets) could be the new way of studying the dynamical evolution of SP comets.

Precise positions of Triton in 2010–2014 based on Gaia-DR2

2021 ◽  
Author(s):  
Huiyan Zhang ◽  
Yong Yu ◽  
Dan Yan ◽  
Kai Tang ◽  
Rongchuan Qiao
Keyword(s):  
Solar System ◽  
Physical Properties ◽  
Orbital Evolution ◽  
Astronomical Observatory ◽  
Standard Errors ◽  
Origin And Evolution ◽  
Important Target ◽  
Long Time ◽  
Gaia Dr2

Abstract With unique orbital and physical characteristics, Triton is a very important target since it may contain information of the origin and evolution of the solar system. Besides space explorations, ground-based observations over long time also play key role on research of Triton. High-precision positions of Triton obtained from ground telescopes are of great significance for studying its orbital evolution and inverting the physical properties of Neptune. As a long-term observational target, Triton has been observed by the 1.56 m telescope of Shanghai Astronomical Observatory since 1996. In this paper, based on our AAPPDI software and with Gaia DR2 as the reference catalogue, 604 positions of Triton during 2010-2014 are calculated, with standard errors of $19mas-88mas$. A comparison between our results and the ephemeris (DE431+nep096) is also given.

Orbits of Trojan Asteroids

1974 ◽  
Vol 62 ◽  
pp. 63-69 ◽  
Author(s):  
G. A. Chebotarev ◽  
N. A. Belyaev ◽  
R. P. Eremenko
Keyword(s):  
Solar System ◽  
Body Problem ◽  
Equations Of Motion ◽  
Orbital Evolution ◽  
Restricted Three Body Problem ◽  
Three Body Problem ◽  
Trojan Asteroids ◽  
Actual Motion ◽  
Three Body

In this paper the orbital evolution of Trojan asteroids are studied by integrating numerically the equations of motion over the interval 1660–2060, perturbations from Venus to Pluto being taken into account. The comparison of the actual motion of Trojans in the solar system with the theory based on the restricted three-body problem are given.

scholarly journals The Locations of Secular Resonances and the Evolution of Small Solar System Bodies

1992 ◽  
Vol 152 ◽  
pp. 123-132
Author(s):  
Ch Froeschle ◽  
P. Farinella ◽  
C. Froeschle ◽  
Z. Knežević ◽  
A. Milani
Keyword(s):  
Perturbation Theory ◽  
Solar System ◽  
Small Body ◽  
Kuiper Belt ◽  
Dynamical Evolution ◽  
Asteroid Belt ◽  
Secular Resonances ◽  
Outer Planets ◽  
Proper Elements ◽  
Solar System Bodies

Generalizing the secular perturbation theory of Milani and Knežević (1990), we have determined in the a — e — I proper elements space the locations of the secular resonances between the precession rates of the longitudes of perihelion and node of a small body and the corresponding eigenfrequencies of the secular perturbations of the four outer planets. We discuss some implications of the results for the dynamical evolution of small solar system bodies. In particular, our findings include: (i) the fact that the g = g6 resonance in the inner asteroid belt lies closer than previously assumed to the Flora region, providing a plausible dynamical route to inject asteroid fragments into planet-crossing orbits; (ii) the possible presence of some low-inclination “stable islands” between the orbits of the outer planets; (iii) the fact that none of the secular resonances considered in this work exists for semimajor axes > 50 AU, so that these resonances do not provide a mechanism for transporting inwards possible Kuiper–belt comets.

scholarly journals Effects of Multiple Planetary Encounters on Kuiper Belt Objects

2002 ◽  
Vol 12 ◽  
pp. 243-244
Author(s):  
Ştefan Berinde
Keyword(s):  
Solar System ◽  
Diffusion Process ◽  
Statistical Approach ◽  
Kuiper Belt ◽  
Giant Planets ◽  
Outer Solar System ◽  
Kuiper Belt Objects ◽  
Easy Task ◽  
Close Encounters ◽  
Long Time

Nowadays many attempts are made to establish a qualitative and a quantitative connection between Kuiper Belt Population and Jupiter Family Comets. Basically, this can be thought as a diffusion process throughout the outer Solar System due to multiple close encounters with the giant planets. But, following the path of a body in such a process is not an easy task to be approached analytically nor numerically, because the motion is very chaotic and spread over a long time. A statistical approach seems to be a reasonable way and is the purpose of this paper.

scholarly journals Dynamical evolution of dense star clusters in galactic nuclei

2013 ◽  
Vol 9 (S303) ◽  
pp. 235-237
Author(s):  
Jaroslav Haas ◽  
Ladislav Šubr
Keyword(s):  
Power Law ◽  
Density Profile ◽  
Surface Density ◽  
Gravitational Interaction ◽  
Dynamical Evolution ◽  
Orbital Evolution ◽  
Stellar Disk ◽  
Central Mass ◽  
Symmetric Star ◽  
Sgr A

AbstractBy means of direct numerical N-body modeling, we investigate the orbital evolution of an initially thin, central mass dominated stellar disk. We include the perturbative gravitational influence of an extended spherically symmetric star cluster and the mutual gravitational interaction of the stars within the disk. Our results show that the two-body relaxation of the disk leads to significant changes of its radial density profile. In particular, the disk naturally evolves, for a variety of initial configurations, a similar broken power-law surface density profile. Hence, it appears that the single power-law surface density profile ∝R−2 suggested by various authors to describe the young stellar disk observed in the Sgr A* region does not match theoretical expectations.

scholarly journals Frequency Map and Global Dynamics in Planetary systems: Short Period Dynamics

2004 ◽  
Vol 202 ◽  
pp. 235-237
Author(s):  
Philippe Robutel ◽  
Jacques Laskar
Keyword(s):  
Solar System ◽  
Degrees Of Freedom ◽  
Kuiper Belt ◽  
Complete Analysis ◽  
Integration Time ◽  
Global Dynamics ◽  
Mean Motion Resonances ◽  
Short Period ◽  
Frequency Map ◽  
Map Analysis

Frequency Map Analysis (FMA) (Laskar, 1990, 1999) is a refined numerical method based on Fourier techniques which provide a clear representation of the global dynamics of multi-dimensional systems, which is very effective for systems of 3 degrees of freedom and more, and was applied to a large class of dynamical systems. FMA requires only a very short integration time to obtain a measure of the diffusion of the trajectories, and allows to identify easily the location of the main resonances. Using this method, we have performed a complete analysis of massless particles in the Solar System (Robutel & Laskar 2001), from Mercury to the outer parts of the Kuiper belt (90 AU), for all values of the eccentricities, and several values for the inclinations. This provides a complete dynamical map of the Solar System, which is, in this first step, restricted to mean motion resonances. The dynamics of a planetary system which all the bodies have no zero mass can be studied with the same methods: an application to the JupiterSaturn system can be fined in (Robutel & Laskar 2002). We present here the application of this method to the understanding of the dynamics of the newly discovered v-Andromedae system.

scholarly journals Dynamical Evolution of the Early Solar System

2018 ◽  
Vol 56 (1) ◽  
pp. 137-174 ◽  
Author(s):  
David Nesvorný
Keyword(s):  
Solar System ◽  
Kuiper Belt ◽  
Dynamical Evolution ◽  
Giant Planets ◽  
Asteroid Belt ◽  
Dynamical Instability ◽  
Orbital Energy ◽  
Interstellar Space ◽  
Early Solar System ◽  
Planetary Migration

Several properties of the Solar System, including the wide radial spacing of the giant planets, can be explained if planets radially migrated by exchanging orbital energy and momentum with outer disk planetesimals. Neptune's planetesimal-driven migration, in particular, has a strong advocate in the dynamical structure of the Kuiper belt. A dynamical instability is thought to have occurred during the early stages with Jupiter having close encounters with a Neptune-class planet. As a result of the encounters, Jupiter acquired its current orbital eccentricity and jumped inward by a fraction of an astronomical unit, as required for the survival of the terrestrial planets and from asteroid belt constraints. Planetary encounters also contributed to capture of Jupiter Trojans and irregular satellites of the giant planets. Here we discuss the dynamical evolution of the early Solar System with an eye to determining how models of planetary migration/instability can be constrained from its present architecture. Specifically, we review arguments suggesting that the Solar System may have originally contained a third ice giant on a resonant orbit between Saturn and Uranus. This hypothesized planet was presumably ejected into interstellar space during the instability. The Kuiper belt kernel and other dynamical structures in the trans-Neptunian region may provide evidence for the ejected planet. We favor the early version of the instability where Neptune migrated into the outer planetesimal disk within a few tens of millions of years after the dispersal of the protosolar nebula. If so, the planetary migration/instability was not the cause of the Late Heavy Bombardment. Mercury's orbit may have been excited during the instability.

ISLAM PADA MASA KESULTANAN BANTEN

ALQALAM ◽  
2015 ◽  
Vol 32 (1) ◽  
pp. 83
Author(s):  
Maftuh Maftuh
Keyword(s):  
Social Life ◽  
Religious Orientation ◽  
Time Span ◽  
Religious Community ◽  
Historical Approach ◽  
Islamic Studies ◽  
The Social ◽  
Long Time ◽  
Islamic Militancy ◽  
Religious Understanding

For many observers, Banten is well known as an area where the population has a strict religious understanding onislamic law. Colonial officials and experts in Islamic studies such as Snouck Hurgronje and GF Pijper, testified that compared to other Muslims across Java , Muslim in Banten and Cirebon were stricter in practicing Islam . The phenomenon of the social life of the religious community in Banten is necessarily formed within a very long time span. This paper traces the root of the formation of public religious understanding ojMuslim in Banten. Using a socio-historical approach, this paper then leads to the conclusion that the sultan of Banten issued policies that had a greater emphasis to the adherence to the Shari'a rather than Sufism. Religious orientation on the fiqh-oriented can explain the Islamic militancy Banten community, as witnessed by the colonial officials, and even still can be seen up to this present moment.Key words: Jslamization, Sultanate, Banten

scholarly journals Resonant trans-Neptunian objects as a source of Jupiter-family comets

2006 ◽  
Vol 2 (S236) ◽  
pp. 31-34
Author(s):  
E. L. Kiseleva ◽  
V. V. Emel'yanenko
Keyword(s):  
Solar System ◽  
Dynamical Evolution ◽  
Early History ◽  
Substantial Contribution ◽  
Outer Solar System ◽  
Symplectic Integrator ◽  
Relative Fraction ◽  
Outward Transport ◽  
Short Period ◽  
History Of

AbstractThe dynamical interrelation between resonant trans-Neptunian objects and short-period comets is studied. Initial orbits of resonant objects are based on computations in the model of the outward transport of objects during Neptune's migration in the early history of the outer Solar system. The dynamical evolution of this population is investigated for 4.5 Gyr, using a symplectic integrator. Our calculations show that resonant trans-Neptunian objects give a substantial contribution to the planetary region. We have estimated that the relative fraction of objects captured per year from the 2/3 resonance to Jupiter-family orbits with perihelion distances q<2.5 AU is 0.4×10−10 near the present epoch.

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