Masses and age of the chemically peculiar double-lined binary
Author
dc.contributor.author
Le Bouquin, J. B.
Author
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Beust, H.
es_CL
Author
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Duvert, G.
es_CL
Author
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Berger, J. P.
es_CL
Author
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Ménard, Francois
es_CL
Author
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Zins, G.
es_CL
Admission date
dc.date.accessioned
2014-01-28T13:58:31Z
Available date
dc.date.available
2014-01-28T13:58:31Z
Publication date
dc.date.issued
2013
Cita de ítem
dc.identifier.citation
A&A 551, A121 (2013)
en_US
Identifier
dc.identifier.other
DOI: 10.1051/0004-6361/201220454
Identifier
dc.identifier.uri
https://repositorio.uchile.cl/handle/2250/126307
General note
dc.description
Artículo de publicación ISI
en_US
Abstract
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Aims.We aim at measuring the stellar parameters of the two chemically peculiar components of the B9.5Vp HgMn + A2 Vm doublelined
spectroscopic binary HD141556 ( Lup), whose period is 15:25 days.
Methods. We combined historical radial velocity measurements with new spatially resolved astrometric observations from
PIONIER/VLTI to reconstruct the three-dimensional orbit of the binary, and thus obtained the individual masses. We fit the available
photometric points together with the flux ratios provided by interferometry to constrain the individual sizes, which we compared
to predictions from evolutionary models.
Results. The individual masses of the components are Ma = 2:84 0:12 M and Mb = 1:94 0:09 M . The dynamical distance
is compatible with the Hipparcos parallax. We find linear stellar radii of Ra = 2:85 0:15 R and Rb = 1:75 0:18 R . This result
validates a posteriori the flux ratio used in previous detailed abundance studies. Assuming coevality, we determine a slightly sub-solar
initial metallicity Z = 0:012 0:003 and an age of (2:8 0:3) 108 years. Finally, our results imply that the primary rotates more
slowly than its synchronous velocity, while the secondary is probably synchronous. We show that strong tidal coupling during the
pre-main sequence evolution followed by a full decoupling at zero-age main sequence provides a plausible explanation for these very
low rotation rates.