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Dynamical Study of the Exoplanet Host Binary System HD 106515
Rica, F. M.; Barrena, R.; Henríquez, J. A.; Pérez, F. M.; Vargas, P.
AA(Astronomical Federation of Extremadura, C/José Martínez Ruíz Azorín, 14, 4° D, Mérida E-06800, Spain), AB(Instituto de Astrofísica de Canarias, C/ Vía Láctea, s/n, La Laguna E-38205, Spain; Departamento de Astrofísica, Universidad de La Laguna, C/ Astrofísico Francisco Sánchez, s/n, La Laguna E-38201, Spain), AC(Grupo de Observadores Astronómicos de Tenerife (GOAT), Spain; La Palma Astronomical Society, C/ A, no 2, Breña Baja E-38712, Spain), AD(Universidad de La Laguna, C/ Astrofísico Francisco Sánchez, s/n, La Laguna E-38201, Spain), AE(Universidad de La Laguna, C/ Astrofísico Francisco Sánchez, s/n, La Laguna E-38201, Spain)
Publications of the Astronomical Society of Australia, Volume 34, id.e004 14 pp. (PASA Homepage)
Publication Date:
Astronomy Keywords:
(stars:) binaries: visual, stars: individual: (HD 106515), stars: kinematics and dynamics, (stars:) planetary systems
Abstract Copyright:
2017: Astronomical Society of Australia
Bibliographic Code:


HD 106515 AB (STF1619 AB) is a high common proper motion and common radial velocity binary star system composed of two G-type bright stars located at 35 pc and separated by about 7 arcsec. This system was observed by the Hipparcos satellite with a precision in distance and proper motion of 3 and 2%, respectively. The system includes a circumprimary planet of nearly 10 Jupiter masses and a semimajor axis of 4.59 AU, discovered using the radial velocity method. The observational arc of 21° shows a small curvature that evidences HD 106515 AB is a gravitationally bound system. This work determines the dynamical parameters for this system which reinforce the bound status of both stellar components. We determine orbital solutions from instantaneous position and velocity vectors. In addition, we provide a very preliminary orbital solution and a distribution of the orbital parameters, obtained from the line of sight (z). Our results show that HD 106515 AB presents an orbital period of about 4 800 years, a semimajor axis of 345 AU and an eccentricity of about 0.42. Finally, we use an N-body numerical code to perform simulations and reproduce the longer term octupole perturbations on the inner orbit.
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