New spectroscopic binary companions of giant stars and updated metallicity distribution for binary systems

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dc.contributor.authorBluhm, P
dc.contributor.authorJones, MI
dc.contributor.authorVanzi, L
dc.contributor.authorSoto, MG
dc.contributor.authorVoss, J
dc.contributor.authorWittenmyer, RA
dc.contributor.authorDrass, H
dc.contributor.authorJenkins, JS
dc.contributor.authorOlivares, F
dc.contributor.authorMennickent, RE
dc.contributor.authorVuckovic, M
dc.contributor.authorRojo, P
dc.contributor.authorMelo, CHF
dc.date.accessioned2017-03-10T13:16:55Z
dc.date.available2017-03-10T13:16:55Z
dc.date.issued2016-09
dc.descriptionIndexación: Web of Sciencees
dc.description.abstractWe report the discovery of 24 spectroscopic binary companions to giant stars. We fully constrain the orbital solution for 6 of these systems. We cannot unambiguously derive the orbital elements for the remaining stars because the phase coverage is incomplete. Of these stars, 6 present radial velocity trends that are compatible with long-period brown dwarf companions. The orbital solutions of the 24 binary systems indicate that these giant binary systems have a wide range in orbital periods, eccentricities, and companion masses. For the binaries with restricted orbital solutions, we find a range of orbital periods of between similar to 97-1600 days and eccentricities of between similar to 0.1-0.4. In addition, we studied the metallicity distribution of single and binary giant stars. We computed the metallicity of a total of 395 evolved stars, 59 of wich are in binary systems. We find a flat distribution for these binary stars and therefore conclude that stellar binary systems, and potentially brown dwarfs, have a different formation mechanism than planets. This result is confirmed by recent works showing that extrasolar planets orbiting giants are more frequent around metal-rich stars. Finally, we investigate the eccentricity as a function of the orbital period. We analyzed a total of 130 spectroscopic binaries, including those presented here and systems from the literature. We find that most of the binary stars with periods. 30 days have circular orbits, while at longer orbital periods we observe a wide spread in their eccentricities.es
dc.description.urihttp://www.aanda.org/articles/aa/abs/2016/09/aa28459-16/aa28459-16.html
dc.identifier.citationA&A 593, A133 (2016)es
dc.identifier.issn1432-0746
dc.identifier.otherhttps://doi.org/10.1051/0004-6361/201628459
dc.identifier.urihttp://repositorio.unab.cl/xmlui/handle/ria/3057
dc.language.isoenes
dc.publisherEDP SCIENCESes
dc.subjectRADIAL-VELOCITY MEASUREMENTSes
dc.subjectSOLAR-TYPE STARSes
dc.subjectPLANET SEARCHes
dc.subjectK-GIANTSes
dc.subjectSYNCHRONIZATIONes
dc.subjectCIRCULARIZATIONes
dc.subjectSPECTROMETERes
dc.subjectMULTIPLICITYes
dc.subjectPRECISIONes
dc.subjectSAMPLEes
dc.titleNew spectroscopic binary companions of giant stars and updated metallicity distribution for binary systemses
dc.typeArtículoes
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