The astrodynamics of new planetary systems - The elliptic restricted 3-body problem

Details The astrodynamics of new planetary systems - The elliptic restricted 3-body problem The astrodynamics of new planetary systems - The elliptic restricted 3-body problem

Jan 1997

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1997aas..meet.....k&link_type=abstract

Conference Paper, AAS Paper 97-735

Astronomy and Astrophysics

Astronomy

Extrasolar Planets, Planetary Systems, Three Body Problem, Elliptical Orbits, Orbit Perturbation, Planetary Orbits, Boundary Conditions, Angular Momentum, Circular Orbits, Brown Dwarf Stars, Jupiter Satellites, Deep Space

Scientific paper

Elliptic restricted three-body problem (ER3BP) simulations illustrate measures of relative stability for extrasolar planets, using terrestrial analogs as 3rd bodies in the 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, plus increments above and below. As tracked for 10 exp 3 to 10 exp 5 years, secondary bodies perturbed nominally circular, co-planar planetary orbits at pericentron passage, causing eccentricity and angular momentum to cycle from 10 exp 2 to 10 exp 5 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 chaotic motions. Effective temperature bounds of stable regions varied with each binary system. For calibrating detection projects, observations of Earth from deep space are suggested.

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