scholarly journals Orbital evolution of dust in the Edgeworth–Kuiper belt zone

2015 ◽  
Vol 450 (1) ◽  
pp. 523-532
Author(s):  
J. Klačka ◽  
M. Kocifaj
Keyword(s):  
Kuiper Belt ◽  
Orbital Evolution

scholarly journals Orbital Evolution of the Kuiper Belt

2005 ◽  
Vol 13 ◽  
pp. 922-922
Author(s):  
Charles Morgan ◽  
Andrew Prentice
Keyword(s):  
Kuiper Belt ◽  
Orbital Evolution ◽  
Narrow Ring

AbstractThe observed distribution of trans-Neptunian objects (TNOs) implies that they originally orbited in a narrow ring of radius 41 AU. The mass of the largest TNO was around 1 — 4 x 1026 g.

scholarly journals DYNAMICAL EFFECTS FROM ASTEROID BELTS FOR PLANETARY SYSTEMS

2004 ◽  
Vol 14 (09) ◽  
pp. 3153-3166 ◽  
Author(s):  
ING-GUEY JIANG ◽  
LI-CHIN YEH
Keyword(s):  
Phase Plane ◽  
Kuiper Belt ◽  
Planetary Systems ◽  
Orbital Evolution ◽  
Outer Edge ◽  
Phase Plane Analysis ◽  
Keplerian Orbit ◽  
Plane Analysis ◽  
Natural Mechanism ◽  
The One

The orbital evolution and stability of planetary systems with interaction from the belts is studied using the standard phase-plane analysis. In addition to the fixed point which corresponds to the Keplerian orbit, there are other fixed points around the inner and outer edges of the belt. Our results show that for the planets, the probability to move stably around the inner edge is larger than the one to move around the outer edge. It is also interesting that there is a limit cycle of semi-attractor for a particular case. Applying our results to the Solar System, we find that our results could provide a natural mechanism to do the orbit rearrangement for the larger Kuiper Belt Objects and thus successfully explain the absence of these objects beyond 50 AU.

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.

The evolution of the Kuiper belt during the formation of the outer planets

1999 ◽  
Vol 173 ◽  
pp. 37-44
Author(s):  
M.D. Melita ◽  
A. Brunini
Keyword(s):  
Kuiper Belt ◽  
Outer Planets ◽  
Self Consistent ◽  
Planetary Bodies ◽  
Mass Depletion

AbstractA self-consistent study of the formation of planetary bodies beyond the orbit of Saturn and the evolution of Kuiper disks is carried out by means of an N-body code where accretion and gravitational encounters are considered. This investigation is focused on the aggregation of massive bodies in the outer planetary region and on the consequences of such process in the corresponding cometary belt. We study the link between the bombardment of massive bodies and mass depletion and eccentricity excitation.

Results in orbital evolution of objects in the geosynchronous region

1990 ◽  
Author(s):  
LARRY FRIESEN ◽  
ALBERT JACKSON, IV ◽  
HERBERT ZOOK ◽  
DONALD KESSLER
Keyword(s):  
Orbital Evolution

scholarly journals A statistical review of light curves and the prevalence of contact binaries in the Kuiper Belt

Icarus ◽  
2021 ◽  
Vol 356 ◽  
pp. 114098
Author(s):  
Mark R. Showalter ◽  
Susan D. Benecchi ◽  
Marc W. Buie ◽  
William M. Grundy ◽  
James T. Keane ◽  
...  
Keyword(s):  
Kuiper Belt ◽  
Light Curves ◽  
Statistical Review ◽  
Contact Binaries

Discovery of the candidate Kuiper belt object 1992 QB1

Nature ◽  
1993 ◽  
Vol 362 (6422) ◽  
pp. 730-732 ◽  
Author(s):  
David Jewitt ◽  
Jane Luu
Keyword(s):  
Kuiper Belt ◽  
Kuiper Belt Object

The Kuiper Belt as a Resonant Cavity

2003 ◽  
Vol 584 (1) ◽  
pp. L39-L42 ◽  
Author(s):  
William R. Ward
Keyword(s):  
Kuiper Belt ◽  
Resonant Cavity

scholarly journals Evolution of the Kuiper Belt during the Accretion of the Outer Planets

2002 ◽  
Vol 12 ◽  
pp. 214-218
Author(s):  
A. Brunini ◽  
M.D. Melita
Keyword(s):  
Kuiper Belt ◽  
Resonance Capture ◽  
Orbital Structure ◽  
Outer Planets ◽  
Self Consistent ◽  
The Impact ◽  
Outward Migration

AbstractA set of self-consistent simulations of the formation of Uranus and Neptune are performed to study the evolution of the native KBOs in the process. Our main goal is to have a deeper understanding of the impact of the formation of the outer planets on the present orbital structure of the trans-neptunian region. We aim to understand if resonance capture driven by the outward migration of Neptune can actually occur and its interplay with the invasion of massive planetesimals expelled from the Uranus-Neptune region as a byproduct of their formation. Also the putative present existence in the Oort reservoir of a population of objects originated in the Kuiper belt is analyzed.

scholarly journals Comets

1998 ◽  
Vol 11 (2) ◽  
pp. 1155-1156
Author(s):  
H.U. Keller
Keyword(s):  
Solar System ◽  
Physical Properties ◽  
Data Reduction ◽  
Kuiper Belt ◽  
Preliminary Results ◽  
Open Time ◽  
Transneptunian Objects ◽  
Selection For

Comets, the most pristine members of our solar system, are faint at large heliocentric distances (rh > 3 au) and therefore difficult to observe. Data reduction of these faint objects (periodic comets) is time consuming and hence most often just preliminary results can be discussed. Only the orbits of short periodic comets can be predicted and most of those that have been accessible for ISO have been covered within the guaranteed time programme. About 10 proposals were accepted by the selection for open time proposals. A target of opportunity team was formed. The outstanding comet Hale-Bopp (C/1995 01), one of the brightest and therefore most active comets of this century, was suggested and accepted as TOO. The important results from the ISO cometary programme are derived from its observations. In addition to the observations of "classic" comets the newly detected (Jewitt and Luu, 1993) transneptunian objects, probably objects from the Kuiper belt, are observed in an attempt to determine their physical properties.

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