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dc.contributor.author
Cowley, C. R.
dc.contributor.author
Hubrig, S.
dc.contributor.author
Gonzalez, Jorge Federico
dc.contributor.author
Savanov, I.
dc.date.available
2017-02-14T16:00:03Z
dc.date.issued
2010-11
dc.identifier.citation
Cowley, C. R.; Hubrig, S.; Gonzalez, Jorge Federico; Savanov, I.; Abundances in the Herbig Ae star HD 101412. Abundance anomalies; λ Boo-Vega characteristics?; Edp Sciences; Astronomy And Astrophysics; 523; 11-2010; 65-71
dc.identifier.issn
0004-6361
dc.identifier.uri
http://hdl.handle.net/11336/12976
dc.description.abstract
Context. Recent attention has been directed to abundance variations among very young stars.
Aims. We perform a detailed abundance study of the Herbig Ae star HD 101412, taking advantage of its unusually sharp spectral lines.
Methods. High-resolution spectra are measured for accurate wavelengths and equivalent widths. Balmer-line fits and ionization equlibria give a relation between Teff, and log (g). Abundance anomalies and uncertain reddening preclude the use of spectral type or photometry to fix Teff. Excitation temperatures are used to break the degeneracy between Teff and log (g).
Results. Strong lines are subject to an anomalous saturation that cannot be removed by assuming a low microturbulence. By restricting the analysis to weak (≤20 mÅ) lines, we find consistent results for neutral and ionized species, based on a model with Teff = 8300 K, and log (g) = 3.8. The photosphere is depleted in the most refractory elements, while volatiles are normal or, in the case of nitrogen, overabundant with respect to the sun. The anomalies are unlike those of Ap or Am stars.
Conclusions. We suggest the anomalous saturation of strong lines arises from heating of the upper atmospheric layers by infalling material from a disk. The overall abundance pattern may be related to those found for the λ Boo stars, though the depletions of the refractory elements are milder, more like those of Vega. However, the intermediate volatile zinc is depleted, precluding a straightforward interpretation of the abundance pattern in terms of gas-grain separation.
dc.format
application/pdf
dc.language.iso
eng
dc.publisher
Edp Sciences
dc.rights
info:eu-repo/semantics/openAccess
dc.rights.uri
https://creativecommons.org/licenses/by-nc-sa/2.5/ar/
dc.subject
Stars: Chemically Peculiar
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Stars: Abundances
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Stars: Pre Main Sequence
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Stars: Early-Type
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Astronomía
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Ciencias Físicas
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CIENCIAS NATURALES Y EXACTAS
dc.title
Abundances in the Herbig Ae star HD 101412. Abundance anomalies; λ Boo-Vega characteristics?
dc.type
info:eu-repo/semantics/article
dc.type
info:ar-repo/semantics/artículo
dc.type
info:eu-repo/semantics/publishedVersion
dc.date.updated
2017-02-13T20:30:28Z
dc.journal.volume
523
dc.journal.pagination
65-71
dc.journal.pais
Francia
dc.description.fil
Fil: Cowley, C. R.. University Of Michigan; Estados Unidos
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Fil: Hubrig, S.. AIP; Alemania
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Fil: Gonzalez, Jorge Federico. Consejo Nacional de Investigaciones Cientificas y Tecnicas. Centro Cientifico Tecnologico San Juan. Instituto de Ciencias Astronomicas de la Tierra y del Espacio; Argentina
dc.description.fil
Fil: Savanov, I.. Russian Academy of Sciences. Institute of Astronomy; Rusia
dc.journal.title
Astronomy And Astrophysics
dc.relation.alternativeid
info:eu-repo/semantics/altIdentifier/doi/http://dx.doi.org/10.1051/0004-6361/201015361
dc.relation.alternativeid
info:eu-repo/semantics/altIdentifier/url/http://www.aanda.org/articles/aa/abs/2010/15/aa15361-10/aa15361-10.html
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