Hostname: page-component-8448b6f56d-dnltx Total loading time: 0 Render date: 2024-04-19T21:47:08.444Z Has data issue: false hasContentIssue false
  • English
  • Français

Stellar Wobble Due to a Nearby Binary System

Published online by Cambridge University Press:  23 April 2012

M. H. M. Morais  and
A. C. M. Correia
M. H. M. Morais
Affiliation:
Department of Physics, I3N, University of Aveiro, Campus Universitario de Santiago, 3810-193 Aveiro, Portugal email: helena.morais@ua.pt
A. C. M. Correia
Affiliation:
Astronomie et Systemes Dynamiques, IMCCE-CNRS UMR 8028, 77 Avenue Denfert-Rochereau, 75014 Paris, France email: correia@ua.pt
Rights & Permissions [Opens in a new window]

Abstract

Core share and HTML view are not available for this content. However, as you have access to this content, a full PDF is available via the ‘Save PDF’ action button.

To date, there are several reported exoplanet detections within binary star systems. These findings are based on radial velocity data for the target star. However, the companion star could in turn have a companion of which we are not aware. We describe how this hidden binary system affects the radial velocity of the target star, mimicking a planet in some circumstances We also explain what can be done in practice in order to distinguish between these two effects.

Keywords

(stars:) binaries: general(stars:) planetary systemstechniques: radial velocities
Type
Contributed Papers
Information
Proceedings of the International Astronomical Union , Volume 7 , Symposium S282: From Interacting Binaries to Exoplanets: Essential Modeling Tools , July 2011 , pp. 137 - 138
Copyright
Copyright © International Astronomical Union 2012

References

[1]Morais, M. H. M. & Correia, A. C. M. 2008, A&A, 391, 899Google Scholar
[2]Morais, M. H. M. & Correia, A. C. M. 2011, A&A, 525, A152Google Scholar
[3]Morais, M. H. M. & Correia, A. C. M. 2011, MNRAS, submittedGoogle Scholar