Stellar and dynamical evolution within triple systems

P. P. Eggleton; L. G. Kiseleva

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arXiv · astro-ph/9510110

Stellar and dynamical evolution within triple systems

P. P. Eggleton·L. G. Kiseleva

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Abstract

About 5-15% of stellar systems are at least triple. About 1% of systems with a primary of $\tgs 1 \Mscun$ are triple with a {\it longer} peri od that is less than 30y, and so may in principle be capable of Roche-lobe overflow in both the inner and the outer orbits, at different times. We discuss possible evolutionary paths for these systems, some of which may lead to objects that are difficult to understand in the context of purely binary evolution. An example is OW Gem, a binary containing two supergiants (spectral types F and G) with masses that difffer by a factor of 1.5. There is also a triple-star pathway which could lead rather naturally to low-mass X-ray binaries; whereas binary pathways often appear rather contrived. We also discuss some dynamical pr ocesses involved in the 3-body problem. A number of triple stars are found in clusters. Similar systems can be created by gravitational capture during N-body simulations of Galactic clusters, especially if there is a n assumed primordial binary population. We discuss the properties of these triples , and note that many can be quite long-lived.

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P. P. Eggleton, L. G. Kiseleva. 1995-10-20. Stellar and dynamical evolution within triple systems. https://arxiv.org/abs/astro-ph/9510110

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