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dc.contributor.author
Netopil, M.  
dc.contributor.author
Fossati, L.  
dc.contributor.author
Paunzen, E.  
dc.contributor.author
Zwintz, K.  
dc.contributor.author
Pintado, Olga Ines  
dc.contributor.author
Bagnulo, S.  
dc.date.available
2017-12-11T22:00:32Z  
dc.date.issued
2014-07  
dc.identifier.citation
Netopil, M.; Fossati, L.; Paunzen, E.; Zwintz, K.; Pintado, Olga Ines; et al.; A probable pre-main sequence chemically peculiar star in the open cluster Stock 16; Oxford University Press; Monthly Notices of the Royal Astronomical Society; 442; 2; 7-2014; 3761-3768  
dc.identifier.issn
0035-8711  
dc.identifier.uri
http://hdl.handle.net/11336/30216  
dc.description.abstract
We used the Ultraviolet and Visual Echelle Spectrograph of the ESO-Very Large Telescope to obtain a high resolution and high signal-to-noise ratio spectrum of Stock 16-12, an early-type star which previous Δa photometric observations suggest being a chemically peculiar (CP) star. We used spectral synthesis to perform a detailed abundance analysis obtaining an effective temperature of 8400 ± 400 K, a surface gravity of 4.1 ± 0.4, a microturbulence velocity of 3.4 +0.7−0.3 −0.3+0.7 km s−1, and a projected rotational velocity of 68 ± 4 km s−1. We provide photometric and spectroscopic evidence showing the star is most likely a member of the young Stock 16 open cluster (age 3–8 Myr). The probable cluster membership, the star's position in the Hertzsprung–Russell diagram, and the found infrared excess strongly suggest the star is still in the pre-main-sequence (PMS) phase. We used PMS evolutionary tracks to determine the stellar mass, which ranges between 1.95 and 2.3 M⊙, depending upon the adopted spectroscopic or photometric data results. Similarly, we obtained a stellar age ranging between 4 and 6 Myr, in agreement with that of the cluster. Because the star's chemical abundance pattern resembles well that known of main sequence CP metallic line (Am) stars, the object sets important constraints to the diffusion theory. Additional spectroscopic and spectropolarimetric data allowed us to conclude that the object is probably a single non-magnetic star.  
dc.format
application/pdf  
dc.language.iso
eng  
dc.publisher
Oxford University Press  
dc.rights
info:eu-repo/semantics/openAccess  
dc.rights.uri
https://creativecommons.org/licenses/by-nc-sa/2.5/ar/  
dc.subject
Stars: Abundances  
dc.subject
Stars: Chemically Peculiar  
dc.subject
Stars: Pre-Main-Sequence  
dc.subject.classification
Astronomía  
dc.subject.classification
Ciencias Físicas  
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CIENCIAS NATURALES Y EXACTAS  
dc.title
A probable pre-main sequence chemically peculiar star in the open cluster Stock 16  
dc.type
info:eu-repo/semantics/article  
dc.type
info:ar-repo/semantics/artículo  
dc.type
info:eu-repo/semantics/publishedVersion  
dc.date.updated
2017-12-11T19:24:18Z  
dc.journal.volume
442  
dc.journal.number
2  
dc.journal.pagination
3761-3768  
dc.journal.pais
Reino Unido  
dc.journal.ciudad
Oxford  
dc.description.fil
Fil: Netopil, M.. Masaryk University; República Checa  
dc.description.fil
Fil: Fossati, L.. Universitaet Bonn; Alemania  
dc.description.fil
Fil: Paunzen, E.. Masaryk University; República Checa  
dc.description.fil
Fil: Zwintz, K.. Katholikie Universiteit Leuven; Bélgica  
dc.description.fil
Fil: Pintado, Olga Ines. Consejo Nacional de Investigaciones Científicas y Técnicas. Centro Científico Tecnológico Conicet - Tucumán. Instituto Superior de Correlación Geológica. Universidad Nacional de Tucumán. Facultad de Ciencias Naturales e Instituto Miguel Lillo. Departamento de Geología. Cátedra Geología Estructural. Instituto Superior de Correlación Geológica; Argentina  
dc.description.fil
Fil: Bagnulo, S.. Armagh Observatory; Irlanda  
dc.journal.title
Monthly Notices of the Royal Astronomical Society  
dc.relation.alternativeid
info:eu-repo/semantics/altIdentifier/doi/http://dx.doi.org/ 10.1093/mnras/stu1130  
dc.relation.alternativeid
info:eu-repo/semantics/altIdentifier/url/https://academic.oup.com/mnras/article/442/4/3761/1362487