AAS 97-735
THE ASTRODYNAMICS OF NEW PLANETARY SYSTEMS: THE ELLIPTIC RESTRICTED 3-BODY PROBLEM
W.D. Kelly - Triton Systems
Abstract
Elliptic Restricted 3-Body Problem (ER3BP) simulations illustrate measures of relative stability for extra-solar planets, using terrestrial analogs as 3rd bodies in binary systems Alpha Centauri, Procyon, Sirius, Jupiter-Sun, 47 Ursae Majoris and 70 Virginis. Initial conditions placed hypothetical planets in nominally circular orbits at Earth analogous radiative flux regions (400 deg K effective stellar temperature at orbital radius ), plus increments above and below. As tracked for 1,000 to 100,000 years, secondary bodies (star, brown dwarf or planet) perturbed nominally circular, co-planar planetary orbits at pericentron passage, causing eccentricity and angular momentum to cycle from 100 to 100,000 years as planet periastron precessed. Cases include satellites of jovian planets or brown dwarfs. Cycle magnitudes and periods varied with star system case and thermal environment. In some instances, stable orbit bounds were established by capture, ejection or advent of chaoti