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dc.creatorDesidera, S.en_US
dc.creatorCarolo, E.en_US
dc.creatorGratton, R.en_US
dc.creatorFiorenzano, A. F. Martinezen_US
dc.creatorEndl, M.en_US
dc.creatorMesa, D.en_US
dc.creatorBarbieri, M.en_US
dc.creatorBonavita, M.en_US
dc.creatorCecconi, M.en_US
dc.creatorClaudi, R. U.en_US
dc.creatorCosentino, R.en_US
dc.creatorMarzari, F.en_US
dc.creatorScuderi, S.en_US
dc.date.accessioned2016-04-22T19:43:59Z
dc.date.available2016-04-22T19:43:59Z
dc.date.issued2011-09en
dc.identifierdoi:10.15781/T2TJ69
dc.identifier.citationDesidera, S., E. Carolo, R. Gratton, AF Martinez Fiorenzano, M. Endl, D. Mesa, M. Barbieri et al. >A giant planet in the triple system HD 132563.> Astronomy & Astrophysics, Vol. 533 (Sep., 2011): A90.en_US
dc.identifier.issn0004-6361en_US
dc.identifier.urihttp://hdl.handle.net/2152/34317
dc.description.abstractAs part of our radial velocity planet-search survey performed with SARG at TNG, we monitored the components of HD 132563 for ten years. It is a binary system formed by two rather similar solar type stars with a projected separation of 4.1 arcsec, which corresponds to 400 AU at the distance of 96 pc. The two components are moderately metal-poor ([Fe/H] = -0.19), and the age of the system is about 5 Gyr. We detected RV variations of HD 132563B with period of 1544 days and semi-amplitude of 26 m/s. From the star characteristics and line profile measurements, we infer their Keplerian origin. Therefore HD 132563B turns out to host a planet with a projected mass m sin i = 1.49 M-J at 2.6 AU with a moderately eccentric orbit (e = 0.22). The planet around HD 132563B is one of the few that are known in triple stellar systems, as we found that the primary HD 132563A is itself a spectroscopic binary with a period longer than 15 years and an eccentricity higher than 0.65. The spectroscopic component was not detected in adaptive-optics images taken with the instrument AdOpt mounted at the TNG, since it expected at a projected separation that was smaller than 0.2 arcsec at the time of our observations. A small excess in K band difference between the components with respect to the difference in V band is compatible with a companion of about 0.55 M-circle dot. A preliminary statistical analysis of when planets occur in triple systems indicate a similar frequency of planets around the isolated component in a triple system, components of wide binaries and single stars. There is no significant iron abundance difference between the components. The lack of stars in binary systems and open clusters showing strong enhancements of iron abundance, which are comparable to the typical metallicity difference between stars with and without giant planets, agrees with the idea that accretion of planetary material producing iron abundance anomalies over 0.1 dex is rare.en_US
dc.description.sponsorshipPRIN-INAF 2008en_US
dc.language.isoEnglishen_US
dc.rightsAdministrative deposit of works to Texas ScholarWorks: This works author(s) is or was a University faculty member, student or staff member; this article is already available through open access or the publisher allows a PDF version of the article to be freely posted online. The library makes the deposit as a matter of fair use (for scholarly, educational, and research purposes), and to preserve the work and further secure public access to the works of the University.en_US
dc.subjectstars: individual: hd 132563en_US
dc.subjectplanetary systemsen_US
dc.subjectbinaries: visualen_US
dc.subjectbinaries: spectroscopicen_US
dc.subjecttechniques: spectroscopicen_US
dc.subjectexoplanet host starsen_US
dc.subjectextra-solar planetsen_US
dc.subjectlow-mass starsen_US
dc.subjectmultipleen_US
dc.subjectsystemsen_US
dc.subjectbinary-systemsen_US
dc.subjectspectroscopic analysisen_US
dc.subjectabundance differenceen_US
dc.subjectcircumbinary planetsen_US
dc.subjectstellar companionsen_US
dc.subjectradial-velocitiesen_US
dc.subjectastronomy & astrophysicsen_US
dc.titleA Giant Planet In The Triple System HD 132563en_US
dc.typeArticleen_US
dc.description.departmentAstronomyen_US
dc.identifier.doi10.1051/0004-6361/201117191en_US
dc.contributor.utaustinauthorEndl, M.en_US
dc.relation.ispartofserialAstronomy & Astrophysicsen_US


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