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Title:
Stellar wobble caused by a nearby binary system: eccentric and inclined orbits
Authors:
Morais, M. H. M.; Correia, A. C. M.
Affiliation:
AA(Department of Physics, I3N, University of Aveiro, Campus Universitário de Santiago, 3810-193 Aveiro, Portugal ), AB(Department of Physics, I3N, University of Aveiro, Campus Universitário de Santiago, 3810-193 Aveiro, Portugal; Astronomie et Systèmes Dynamiques, IMCCE-CNRS UMR 8028, 77 Avenue Denfert-Rochereau, 75014 Paris, France)
Publication:
Astronomy and Astrophysics, Volume 525, id.A152, 10 pp. (A&A Homepage)
Publication Date:
01/2011
Origin:
EDP Sciences
Astronomy Keywords:
technique: radial velocities, celestial mechanics, planetary systems, binaries: general
DOI:
10.1051/0004-6361/201014812
Bibliographic Code:
2011A&A...525A.152M

Abstract

Most extrasolar planets currently known were discovered by means of an indirect method that measures the stellar wobble caused by the planet. We previously studied a triple system composed of a star and a nearby binary on circular coplanar orbits. We showed that although the effect of the binary on the star can be differentiated from the stellar wobble caused by a planet, because of observational limitations the two effects may often remain indistinguishable. Here, we develop a model that applies to eccentric and inclined orbits. We show that the binary's effect is more likely to be mistaken by planet(s) in the case of coplanar motion observed equator-on. Moreover, when the orbits are eccentric, the magnitude of the binary's effect may be larger than in the circular case. Additionally, an eccentric binary can mimic two planets with orbital periods in the ratio 2/1. However, when the star's orbit around the binary's center of mass has a high eccentricity and a reasonably well-constrained period, it should be easier to distinguish the binary's effect from a planet.
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