Journal Article

On the onset of runaway stellar collisions in dense star clusters – II. Hydrodynamics of three-body interactions

Evghenii Gaburov, James C. Lombardi and Simon Portegies Zwart

in Monthly Notices of the Royal Astronomical Society

Published on behalf of The Royal Astronomical Society

Volume 402, issue 1, pages 105-126
Published in print February 2010 | ISSN: 0035-8711
Published online February 2010 | e-ISSN: 1365-2966 | DOI: http://dx.doi.org/10.1111/j.1365-2966.2009.15900.x
On the onset of runaway stellar collisions in dense star clusters – II. Hydrodynamics of three-body interactions

More Like This

Show all results sharing this subject:

  • Astronomy and Astrophysics

GO

Show Summary Details

Preview

The onset of runaway stellar collisions in young star clusters is more likely to initiate with an encounter between a binary and a third star than between two single stars. Using the initial conditions of such three-star encounters from direct N-body simulations, we model the resulting interaction by means of smoothed particle hydrodynamics (SPH). Our code implements new equations of motion that allow for efficient use of non-equal mass particles and is capable of evolving contact binaries for thousands of orbits, if not indefinitely. We find that, in the majority of the cases considered, all three stars merge together. In addition, we compare our SPH calculations against those of the sticky-sphere approximation. If one is not concerned with mass loss, then the sticky sphere approach gives the correct qualitative outcome in approximately 75 per cent of the cases considered. Among those cases in which the sticky-sphere algorithm identifies only two particular stars to collide, the hydrodynamic calculations find the same qualitative outcome in about half of the instances. If the sticky-sphere approach determines that all three stars merge, then the hydrodynamic simulations invariably agree. However, in such three-star mergers, the hydrodynamic simulations reveal that: (i) mass lost as ejecta can be a considerable fraction of the total mass in the system (up to ∼25 per cent); (ii) due to asymmetric mass loss, the collision product can sometimes receive a kick velocity that exceeds 10 km s−1, large enough to allow the collision product to escape the core of the cluster; and (iii) the energy of the ejected matter can be large enough (up to ∼3 × 1050 erg) to remove or disturb the inter cluster gas appreciably.

Keywords: gravitation; hydrodynamics; methods: numerical; binaries: general

Journal Article.  11663 words.  Illustrated.

Subjects: Astronomy and Astrophysics

Full text: subscription required

How to subscribe Recommend to my Librarian

Users without a subscription are not able to see the full content. Please, subscribe or login to access all content.