S. Portegies Zwart
- On the origin of high-velocity runaway stars
- Monthly Notices of the Royal Astronomical Society
- Volume | Issue number
- 396 | 1
- Pages (from-to)
- Document type
- Faculty of Science (FNWI)
- Anton Pannekoek Institute for Astronomy (API)
We explore the hypothesis that some high-velocity runaway stars attain their peculiar velocities in the course of exchange encounters between hard massive binaries and a very massive star (either an ordinary 50-100 M-circle dot star or a more massive one, formed through runaway mergers of ordinary stars in the core of a young massive star cluster). In this process, one of the binary components becomes gravitationally bound to the very massive star, while the second one is ejected, sometimes with a high speed. We performed three-body scattering experiments and found that early B-type stars (the progenitors of the majority of neutron stars) can be ejected with velocities of greater than or similar to 200-400 km s(-1) (typical of pulsars), while 3-4 M-circle dot stars can attain velocities of greater than or similar to 300-400 km s(-1) (typical of the bound population of halo late B-type stars). We also found that the ejected stars can occasionally attain velocities exceeding the Milky Ways's escape velocity.
- go to publisher's site
- DOI: 10.1111/j.1365-2966.2009.14809.x; eprintid: arXiv:0903.0738
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