Speaker
Description
Star systems containing three stars are common in the universe, with the triple fraction increasing with the mass of the star. Approximately 10% of solar-type stars reside in triples, while this fraction goes up to 60% for 10 stars of 10 solar masses. To fully understand the evolution of massive stars, triple evolution should be taken into account. One of the evolutionary pathways for triples is dynamical instability, in which stellar winds or mass transfer can destabilize the orbits, resulting in disintegration of the triple. In this talk I will present the results of n-body simulations of massive, unstable triples. I will show how these systems can produce collisions between massive stars, or high-velocity massive runaways. I will present the estimated rates for these events, and discuss it in the context of potential observational counterparts.
| Affliation | Anton Pannekoek Institute for Astronomy, University of Amsterdam |
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| Current Position | PhD Student |
