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Stability of outer planetary orbits around binary stars - A comparison of Hill's and Laplace's stability criteriaA comparison is made between the stability criteria of Hill and that of Laplace to determine the stability of outer planetary orbits encircling binary stars. The restricted, analytically determined results of Hill's method by Szebehely and coworkers and the general, numerically integrated results of Laplace's method by Graziani and Black (1981) are compared for varying values of the mass parameter mu. For mu = 0 to 0.15, the closest orbit (lower limit of radius) an outer planet in a binary system can have and still remain stable is determined by Hill's stability criterion. For mu greater than 0.15, the critical radius is determined by Laplace's stability criterion. It appears that the Graziani-Black stability criterion describes the critical orbit within a few percent for all values of mu.
Document ID
19930063308
Document Type
Reprint (Version printed in journal)
External Source(s)
Authors
Kubala, A.
(NASA Headquarters Washington, DC United States)
Black, D.
(Lunar and Planetary Inst. Houston, TX, United States)
Szebehely, V.
(Texas Univ. Austin, United States)
Date Acquired
August 16, 2013
Publication Date
June 1, 1993
Publication Information
Publication: Celestial Mechanics and Dynamical Astronomy
Volume: 56
Issue: 2-Jan
ISSN: 0923-2958
Subject Category
Astrophysics
Accession Number
93A47305
Funding Number(s)
CONTRACT_GRANT: NASW-4574
Distribution Limits
Public
Copyright
Other

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