Stability of Triple Star Systems with Highly Inclined Orbits

Abstract

It is well established that certain detached eclipsing binary stars exhibit apsidal motions whose value is in disagreement with with calculated deviations from Keplerian motion based on tidal effects and the general theory of relativity. Although many theoretical senarios have been demonstrated to bring calculations into line with observations, all have seemed unlikely for various reasons. In particular, it has been established that the hypothesis of a third star in an orbit almost perpendicular to the orbital plane of the close binary system can explain the anomalous motion in at least some cases. The stability of triple star systems with highly inclined orbits has been in doubt, however. We have found conditions which allow the long term stability of such systems so that the third body hypothesis now seems a likely resolution of the apsidal motion problem. We apply our stability criteria to the cases of AS Cam and DI Her and recommend observations at the new Keck interferometer which should be able to directly observe the third bodies in these systems.

arXiv commentedited to match published version

References in corpus (1)

• Observations of the unusual counterpart to the X-ray pulsar AX J0051-733

Cited by in corpus (4)

• First Stars XI. Chemical composition of the extremely metal-poor dwarfs in the binary CS 22876--032
• Tidal and rotational effects in the perturbations of hierarchical triple stellar systems. II. Eccentric systems - the case of AS Camelopardalis
• Apsidal motion of the eclipsing binary AS Camelopardalis: discrepancy resolved
• The evolution of the eccentricity in the eclipsing binary system AS Camelopardalis