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Most extrasolar planets currently known were discovered by means of anindirect method that measures the stellar wobble caused by the planet. Wepreviously studied a triple system composed of a star and a nearby binary oncircular coplanar orbits. We showed that although the effect of the binary onthe star can be differentiated from the stellar wobble caused by a planet,because of observational limitations the two effects may often remainindistinguishable. Here, we develop a model that applies to eccentric andinclined orbits. We show that the binary's effect is more likely to be mistakenby planet(s) in the case of coplanar motion observed equator-on. Moreover, whenthe orbits are eccentric, the magnitude of the binary's effect may be largerthan in the circular case. Additionally, an eccentric binary can mimic twoplanets with orbital periods in the ratio 2/1. However, when the star's orbitaround the binary's center of mass has a high eccentricity and a reasonablywell-constrained period, it should be easier to distinguish the binary's effectfrom a planet.

Stellar wobble caused by a nearby binary system: eccentric and inclined orbits