Planetary orbits in binary stars.
Abstract
Numerical integrations of the general threebody problem, with one component having a planetary mass, indicate that stable planetary orbits can exist in binary stars. The limitation for stability is that the ratio of the periastron distance of the outer tertiary component to the semimajor axis of the close component be somewhere in the range 34, regardless of which of the components is the planet. For most known binaries, this region of stability includes the region of habitability for planets.
 Publication:

The Astronomical Journal
 Pub Date:
 September 1977
 DOI:
 10.1086/112121
 Bibcode:
 1977AJ.....82..753H
 Keywords:

 Binary Stars;
 Celestial Mechanics;
 Extraterrestrial Life;
 Planetary Orbits;
 Three Body Problem;
 Astrometry;
 Circular Orbits;
 Eccentricity;
 Habitability;
 Motion Stability;
 Numerical Integration;
 Planetary Environments;
 Solar System;
 Astronomy