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Hypervelocity planets and transits around hypervelocity stars
Article first published online: 23 APR 2012
DOI: 10.1111/j.1365-2966.2012.20930.x
© 2012 The Authors Monthly Notices of the Royal Astronomical Society © 2012 RAS
Issue
Monthly Notices of the Royal Astronomical Society
Volume 423, Issue 1, pages 948–954, June 2012
Additional Information
How to Cite
Ginsburg, I., Loeb, A. and Wegner, G. A. (2012), Hypervelocity planets and transits around hypervelocity stars. Monthly Notices of the Royal Astronomical Society, 423: 948–954. doi: 10.1111/j.1365-2966.2012.20930.x
Publication History
- Issue published online: 30 MAY 2012
- Article first published online: 23 APR 2012
- Accepted 2012 March 14. Received 2012 March 13; in original form 2012 January 6
- Abstract
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- References
- Cited By
Keywords:
- black hole physics;
- binaries: close;
- binaries: general;
- Galaxy: centre;
- Galaxy: kinematics and dynamics
ABSTRACT
The disruption of a binary star system by the massive black hole at the Galactic Centre, SgrA*, can lead to the capture of one star around SgrA* and the ejection of its companion as a hypervelocity star (HVS). We consider the possibility that these stars may have planets and study the dynamics of these planets. Using a direct N-body integration code, we simulated a large number of different binary orbits around SgrA*. For some orbital parameters, a planet is ejected at a high speed. In other instances, a HVS is ejected with one or more planets orbiting around it. In these cases, it may be possible to observe the planet as it transits the face of the star. A planet may also collide with its host star. In such cases the atmosphere of the star will be enriched with metals. In other cases, a planet is tidally disrupted by SgrA*, leading to a bright flare.