Some Perturbed Keplerian Systems

2012 ◽  
pp. 229-264
Author(s):  
Bruno Cordani
Keyword(s):  
Keplerian Systems

scholarly journals Normal Forms for Perturbed Keplerian Systems

2002 ◽  
Vol 180 (2) ◽  
pp. 471-519 ◽  
Author(s):  
Jesús Palacián
Keyword(s):  
Normal Forms ◽  
Keplerian Systems

Reduced 4D oscillators and orbital elements in Keplerian systems: Cushman–Deprit coordinates

2020 ◽  
Vol 132 (11-12) ◽  
Author(s):  
S. Ferrer ◽  
F. Crespo ◽  
J. L. Zapata
Keyword(s):  
Orbital Elements ◽  
Keplerian Systems

scholarly journals Mission design through averaging of perturbed Keplerian systems: the paradigm of an Enceladus orbiter

2010 ◽  
Vol 108 (1) ◽  
pp. 1-22 ◽  
Author(s):  
Martín Lara ◽  
Jesús F. Palacián ◽  
Ryan P. Russell
Keyword(s):  
Mission Design ◽  
Keplerian Systems

Coordinates for perturbed keplerian systems with axial symmetry

1992 ◽  
Vol 53 (1) ◽  
Author(s):  
Sebasti�n Ferrer ◽  
BruceR. Miller
Keyword(s):  
Axial Symmetry ◽  
Keplerian Systems

scholarly journals The secular evolution of discrete quasi-Keplerian systems

2018 ◽  
Vol 609 ◽  
pp. A38 ◽  
Author(s):  
J.-B. Fouvry ◽  
C. Pichon ◽  
P.-H. Chavanis
Keyword(s):  
Black Hole ◽  
Landau Equation ◽  
Collective Effects ◽  
Galactic Centre ◽  
Central Black Hole ◽  
Massive Black Hole ◽  
Secular Evolution ◽  
Gauss Method ◽  
And Diffusion ◽  
Keplerian Systems

A discrete self-gravitating quasi-Keplerian razor-thin axisymmetric stellar disc orbiting a massive black hole sees its orbital structure diffuse on secular timescales as a result of a self-induced resonant relaxation. In the absence of collective effects, such a process is described by the recently derived inhomogeneous multi-mass degenerate Landau equation. Relying on Gauss’ method, we computed the associated drift and diffusion coefficients to characterise the properties of the resonant relaxation of razor-thin discs. For a disc-like configuration in our Galactic centre, we showed how this secular diffusion induces an adiabatic distortion of orbits and estimate the typical timescale of resonant relaxation. When considering a disc composed of multiple masses similarly distributed, we have illustrated how the population of lighter stars will gain eccentricity, driving it closer to the central black hole, provided the distribution function increases with angular momentum. The kinetic equation recovers as well the quenching of the resonant diffusion of a test star in the vicinity of the black hole (the “Schwarzschild barrier”) as a result of the divergence of the relativistic precessions. The dual stochastic Langevin formulation yields consistent results and offers a versatile framework in which to incorporate other stochastic processes.

Alternative Reduction by Stages of Keplerian Systems. Positive, Negative, and Zero Energy

2020 ◽  
Vol 19 (2) ◽  
pp. 1525-1539 ◽  
Author(s):  
Francisco Crespo ◽  
Sebastián Ferrer
Keyword(s):  
Zero Energy ◽  
Keplerian Systems

On the normalization of perturbed Keplerian systems

1994 ◽  
Vol 107 ◽  
pp. 1900 ◽  
Author(s):  
M. K. M. Ahmed
Keyword(s):  
Keplerian Systems

Simplifications toward Integrability of Perturbed Keplerian Systems

1988 ◽  
Vol 536 (1 Integrability) ◽  
pp. 127-139 ◽  
Author(s):  
SEBASTIAN FERRER ◽  
CAROL A. WILLIAMS
Keyword(s):  
Keplerian Systems

An improved and generalized theory for the collisional evolution of Keplerian systems

1978 ◽  
Vol 58 (2) ◽  
pp. 477-519 ◽  
Author(s):  
K. A. H�meen-Anttila
Keyword(s):  
Keplerian Systems ◽  
Collisional Evolution
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