Astronomy and Astrophysics – Astronomy
Scientific paper
Jun 1993
adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1993cemda..56...51k&link_type=abstract
Celestial Mechanics and Dynamical Astronomy (ISSN 0923-2958), vol. 56, no. 1-2, p. 51-68.
Astronomy and Astrophysics
Astronomy
11
Binary Stars, Hill Method, Laplace Equation, Planetary Orbits, Systems Stability, Motion Stability, Planetary Systems, Three Body Problem
Scientific paper
A 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.
Black David
Kubala A.
Szebehely Vector
No associations
LandOfFree
Stability of outer planetary orbits around binary stars - A comparison of Hill's and Laplace's stability criteria does not yet have a rating. At this time, there are no reviews or comments for this scientific paper.
If you have personal experience with Stability of outer planetary orbits around binary stars - A comparison of Hill's and Laplace's stability criteria, we encourage you to share that experience with our LandOfFree.com community. Your opinion is very important and Stability of outer planetary orbits around binary stars - A comparison of Hill's and Laplace's stability criteria will most certainly appreciate the feedback.
Profile ID: LFWR-SCP-O-1739532