N-parametric canonical perturbation method based on Lie transforms. Application to the analysis of perturbations on multiple stellar systems

2010 ◽  
Author(s):  
Manuel Andrade ◽  
Manuel de León ◽  
D. M. de Diego ◽  
R. M. Ros
Keyword(s):  
Perturbation Method ◽  
Stellar Systems ◽  
Lie Transforms ◽  
Canonical Perturbation

scholarly journals New Approach to the Planetary Theory

1979 ◽  
Vol 81 ◽  
pp. 69-72 ◽  
Author(s):  
Manabu Yuasa ◽  
Gen'ichiro Hori
Keyword(s):  
Perturbation Method ◽  
Canonical Form ◽  
Equations Of Motion ◽  
Disturbing Function ◽  
Averaging Principle ◽  
The Sun ◽  
Planetary Theory ◽  
New Approach ◽  
Canonical Perturbation ◽  
Relative Coordinates

A new approach to the planetary theory is examined under the following procedure: 1) we use a canonical perturbation method based on the averaging principle; 2) we adopt Charlier's canonical relative coordinates fixed to the Sun, and the equations of motion of planets can be written in the canonical form; 3) we adopt some devices concerning the development of the disturbing function. Our development can be applied formally in the case of nearly intersecting orbits as the Neptune-Pluto system. Procedure 1) has been adopted by Message (1976).

An extended canonical perturbation method

1973 ◽  
Vol 7 (1) ◽  
pp. 77-90 ◽  
Author(s):  
J. S. Choi ◽  
B. D. Tapley
Keyword(s):  
Perturbation Method ◽  
Canonical Perturbation

Nonlinear Resonances in a Column Subjected to a Constant End Force

1980 ◽  
Vol 47 (2) ◽  
pp. 409-414 ◽  
Author(s):  
M. R. M. Crespo da Silva
Keyword(s):  
Perturbation Method ◽  
Analytical Determination ◽  
Free Oscillations ◽  
Integrals Of Motion ◽  
Galerkin’S Method ◽  
Galerkin's Method ◽  
Nonlinear Resonances ◽  
Canonical Perturbation

A canonical perturbation method based on Hamilton-Jacobi theory, used together with Galerkin’s method, is employed to analyze the nonlinearly coupled transverse free oscillations of columns subjected to a constant end force. Integrals of motion, readily obtained from this type of analysis, are used to allow the analytical determination of the main characteristics of the resonant motion and of the region of resonance of the system.

scholarly journals Application of first-order canonical perturbation method with dissipative Hori-like kernel

2017 ◽  
Vol 90 ◽  
pp. 11-20 ◽  
Author(s):  
Tomás Baenas ◽  
Alberto Escapa ◽  
José M. Ferrándiz ◽  
Juan Getino
Keyword(s):  
Perturbation Method ◽  
First Order ◽  
Canonical Perturbation

Desiderata in connection by the calibration of the MK-system

1966 ◽  
Vol 24 ◽  
pp. 348-349
Author(s):  
Th. Schmidt-Kaler
Keyword(s):  
Absolute Magnitude ◽  
Review Article ◽  
Stellar Systems ◽  
Astronomical Data ◽  
Intrinsic Colour

This is only an informal remark about some difficulties I am worrying about.I have tried to recalibrate the MK system in terms of intrinsic colour (B–V)0and absolute magnitudeMv. The procedures used have been described in a review article by Voigt (Mitt. Astr. Ges.1963, p. 25–35), and the results for stars of the luminosity classes Ia-O,I and II have been given also in Blaauw's article on the calibration of luminosity criteria in vol. III (Basic Astronomical Data, p. 401) ofStars and Stellar Systems.

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