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Title:
Precession due to a close binary system: an alternative explanation for nu-Octantis?
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:
Monthly Notices of the Royal Astronomical Society, Volume 419, Issue 4, pp. 3447-3456. (MNRAS Homepage)
Publication Date:
02/2012
Origin:
WILEY
Astronomy Keywords:
methods: analytical, techniques: radial velocities, celestial mechanics, planets and satellites: detection, planets and satellites: dynamical evolution and stability, binaries: spectroscopic
Abstract Copyright:
© 2011 The Authors Monthly Notices of the Royal Astronomical Society © 2011 RAS
DOI:
10.1111/j.1365-2966.2011.19986.x
Bibliographic Code:
2012MNRAS.419.3447M

Abstract

We model the secular evolution of a star's orbit when it has a nearby binary system . We assume a hierarchical triple system where the inter-binary distance is small in comparison with the distance to the star. We show that the major secular effect is precession of the star's orbit around the binary system's centre of mass. We explain how we can obtain this precession rate from the star's radial velocity data, and thus infer the binary system's parameters. We show that the secular effect of a nearby binary system on the star's radial velocity can sometimes mimic a planet. We analyse the radial velocity data for nu-Octantis A which has a nearby companion (nu-Octantis B) and we obtain retrograde precession of -0?86 ± 0?02 yr-1. We show that if nu-Octantis B was itself a double star, it could mimic a signal with similarities to that previously identified as a planet of nu-Octantis A. Nevertheless, we need more observations in order to decide in favour of the double-star hypothesis.
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