scholarly journals Three-body orbital stability criteria for circular orbits

1992 ◽  
Vol 254 (1) ◽  
pp. 21-26 ◽  
Author(s):  
J. R. Donnison ◽  
D. F. Mikulskis
Keyword(s):  
Orbital Stability ◽  
Stability Criteria ◽  
Circular Orbits ◽  
Three Body

scholarly journals Orbital stability of high inclination asteroids

1996 ◽  
Vol 172 ◽  
pp. 187-192
Author(s):  
N. A. Solovaya ◽  
E. M. Pittich
Keyword(s):  
Solar System ◽  
Body Problem ◽  
Equations Of Motion ◽  
Orbital Stability ◽  
Dynamical Model ◽  
Restricted Three Body Problem ◽  
Three Body Problem ◽  
Three Body

The orbital evolutions of fictitious asteroids with high inclinations have been investigated. The selected initial orbits represent asteroids with movement, which corresponds to the conditions of the Tisserand invariant for C = C (L1) in the restricted three body problem. Initial eccentricities of the orbits cover the interval 0.0–0.4, inclinations the interval 40–80°, and arguments of perihelion the interval 0–360°. The equations of motion of the asteroids were numerically integrated from the epoch March 25, 1991 forward within the interval of 20,000 years, using a dynamical model of the solar system consisting of all planets. The orbits of the model asteroids are stable at least during the investigated period.

scholarly journals Orbital Evolution of Planetary Systems

2004 ◽  
Vol 202 ◽  
pp. 175-177
Author(s):  
Tapan K. Chatterjee ◽  
V. B. Magalinsky
Keyword(s):  
Solar System ◽  
Ground State ◽  
Minimum Energy ◽  
Orbital Stability ◽  
Planetary Systems ◽  
Active Role ◽  
Orbital Evolution ◽  
Circular Orbits ◽  
Tidal Forces

It is significant that the orbits of the planets in the solar system are very nearly circular, except for Mercury and Pluto where, conceivably, due to their comparatively small sizes, the tidal forces have played a less active role. Most of the suspected planets orbiting pulsars have nearly circular orbits. These systems tend to have minimum energy and are subjected to tidal forces. We find that a planet circularizes its orbit, in an effort to attain orbital stability and the ground state. Details can be found in Magalinsky & Chatterjee, 1997, and Magalinsky and Chatterjee, 2000.

scholarly journals The orbital stability of a test body motion in the field of two massive bodies

2018 ◽  
Vol 168 ◽  
pp. 04001
Author(s):  
Medeu Abishev ◽  
Saken Toktarbay ◽  
Aigerim Abylayeva ◽  
Amanhan Talkhat
Keyword(s):  
Body Problem ◽  
Orbital Stability ◽  
Test Body ◽  
Body Motion ◽  
Restricted Three Body Problem ◽  
Three Body Problem ◽  
Test Particles ◽  
The Stability ◽  
Three Body ◽  
Insight Into

We investigate the orbital stability of a test particle motion in the restricted three-body problem where all bodies have their own rotation. We have shown that it is possible to get some insight into the stability properties of the motion of test particles in restricted three-body problem, without knowing the exact solutions of the relativistic motion equations.

scholarly journals The orbital stability of relativistic three-body problem in the fremework of general relativity

2019 ◽  
Vol 69 (2) ◽  
pp. 53-60
Author(s):  
A.Z. Talkhat ◽  
◽  
A.Zh. Abylayeva ◽  
A. Muratkhan ◽  
◽  
...  
Keyword(s):  
General Relativity ◽  
Body Problem ◽  
Orbital Stability ◽  
Three Body Problem ◽  
Three Body
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