The origin of the Kirkwood gaps - A mapping for asteroidal motion near the 3/1 commensurability

1982 ◽  
Vol 87 ◽  
pp. 577 ◽  
Author(s):  
J. Wisdom
Keyword(s):  
Kirkwood Gaps ◽  
Asteroidal Motion

scholarly journals Resonant Asteroidal Motion in the Kirkwood Gaps: A Three-Dimensional Study

1983 ◽  
Vol 74 ◽  
pp. 163-163
Author(s):  
H. Scholl ◽  
C. Froeschle
Keyword(s):  
Three Dimensional ◽  
Planar Problem ◽  
Dimensional Model ◽  
Three Dimensional Model ◽  
Planar Case ◽  
Kirkwood Gaps ◽  
Elliptical Model ◽  
Asteroidal Motion

AbstractResonant asteroidal motion is investigated over 17 000 years in a three-dimensional elliptical model Sun-Jupiter-Asteroid averaged by Schubart's method à la Poincarè. Orbits remain trapped in the resonance over this period. The various stability mechanisms are discussed. With respect to their behaviour of ω and ῶ, our resulting orbits reveal 5 distinct classes. These 5 classes can be described in Schubart's topology for the planar problem. As compared to the planar case, eccentricities of orbits in the three-dimensional model vary more strongly. This is an important result for the problem of the delivery of meteorites.

On the alleged collisional origin of the Kirkwood gaps

Icarus ◽  
1975 ◽  
Vol 26 (3) ◽  
pp. 367-376 ◽  
Author(s):  
T.A. Heppenheimer
Keyword(s):  
Kirkwood Gaps

Concerning Brouwer's paper on the Kirkwood Gaps

1966 ◽  
Vol 71 ◽  
pp. 543 ◽  
Author(s):  
Dirk Brouwer ◽  
William H. Jefferys
Keyword(s):  
Kirkwood Gaps

scholarly journals Stability of Asteroid Motions

1992 ◽  
Vol 152 ◽  
pp. 115-122
Author(s):  
Y. Kozai
Keyword(s):  
Dynamical Evolution ◽  
Secular Perturbations ◽  
The Past ◽  
Kirkwood Gaps ◽  
Present Distribution

In this paper the author presents evidences showing that for most of the asteroids the motions are stable in the sense that they never approach major planets very closely and explains about mechanisms to avoid very close approaches by investigating the variations due to the secular perturbations of the eccentricities as functions of the arguments of perihelion, particularly, for asteroids with high eccentricities and inclinations. It is believed that some kinds of dynamical evolution processes have made the asteroid motions stable. The author shows also that there were some kinds of collisions among asteroids in the past which produced families and present distribution of asteroids as there are very faint asteroids only near Kirkwood gaps.

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