On the line shift and oscillator strength of Xe II lines in the spectra of HnMn stars

Autores
Di Rocco, Héctor O.; Cruzado, Alicia; Marchiano, Paula Esther
Año de publicación
2015
Idioma
inglés
Tipo de recurso
artículo
Estado
versión publicada
Descripción
Aims. The ultimate goal that has motivated this work is to achieve realistic oscillator strength (gf) values to find reliable values of stellar abundances. We aim to compare the gf valúes of Xe ii lines found with different theoretical and experimental methods. Methods. We have undertaken calculations using the quasirelativistic and relativistic Hartree-Fock methods. Then we compare these results with those previously obtained from UVES spectra of HgMn stars. Results. 1) Our theoretical gf values are more realistic than those previously obtained for most lines. When we consider only unblended, isolated, relatively noise-free lines, however, our theoretical gf values and Yuce's stellar values differ little from each other. 2) In a discussion of the origin of the previously observed discrepancy between the wavelengths of Xe ii lines deducted from stellar spectra and those published by National Institute of Standards and Technology (NIST), we conclude that stellar wavelengths could be considered the standard wavelengths whenever the densities in stellar atmospheres are smaller than 1 × 1016 part. cm-3.
Facultad de Ciencias Astronómicas y Geofísicas
Instituto de Astrofísica de La Plata
Materia
Ciencias Astronómicas
Atomic data
Line: identification
Stars: abundances
Stars: chemically peculiar
Nivel de accesibilidad
acceso abierto
Condiciones de uso
http://creativecommons.org/licenses/by-nc-sa/4.0/
Repositorio
SEDICI (UNLP)
Institución
Universidad Nacional de La Plata
OAI Identificador
oai:sedici.unlp.edu.ar:10915/86392

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oai_identifier_str oai:sedici.unlp.edu.ar:10915/86392
network_acronym_str SEDICI
repository_id_str 1329
network_name_str SEDICI (UNLP)
spelling On the line shift and oscillator strength of Xe II lines in the spectra of HnMn starsDi Rocco, Héctor O.Cruzado, AliciaMarchiano, Paula EstherCiencias AstronómicasAtomic dataLine: identificationStars: abundancesStars: chemically peculiarAims. The ultimate goal that has motivated this work is to achieve realistic oscillator strength (<i>gf</i>) values to find reliable values of stellar abundances. We aim to compare the <i>gf</i> valúes of Xe ii lines found with different theoretical and experimental methods. Methods. We have undertaken calculations using the quasirelativistic and relativistic Hartree-Fock methods. Then we compare these results with those previously obtained from UVES spectra of HgMn stars. Results. 1) Our theoretical <i>gf</i> values are more realistic than those previously obtained for most lines. When we consider only unblended, isolated, relatively noise-free lines, however, our theoretical <i>gf</i> values and Yuce's stellar values differ little from each other. 2) In a discussion of the origin of the previously observed discrepancy between the wavelengths of Xe ii lines deducted from stellar spectra and those published by National Institute of Standards and Technology (NIST), we conclude that stellar wavelengths could be considered the standard wavelengths whenever the densities in stellar atmospheres are smaller than 1 × 10<SUP>16</SUP> part. cm<SUP>-3</SUP>.Facultad de Ciencias Astronómicas y GeofísicasInstituto de Astrofísica de La Plata2015info:eu-repo/semantics/articleinfo:eu-repo/semantics/publishedVersionArticulohttp://purl.org/coar/resource_type/c_6501info:ar-repo/semantics/articuloapplication/pdfhttp://sedici.unlp.edu.ar/handle/10915/86392enginfo:eu-repo/semantics/altIdentifier/issn/0004-6361info:eu-repo/semantics/altIdentifier/doi/10.1051/0004-6361/201526301info:eu-repo/semantics/openAccesshttp://creativecommons.org/licenses/by-nc-sa/4.0/Creative Commons Attribution-NonCommercial-ShareAlike 4.0 International (CC BY-NC-SA 4.0)reponame:SEDICI (UNLP)instname:Universidad Nacional de La Platainstacron:UNLP2025-09-29T11:16:54Zoai:sedici.unlp.edu.ar:10915/86392Institucionalhttp://sedici.unlp.edu.ar/Universidad públicaNo correspondehttp://sedici.unlp.edu.ar/oai/snrdalira@sedici.unlp.edu.arArgentinaNo correspondeNo correspondeNo correspondeopendoar:13292025-09-29 11:16:54.581SEDICI (UNLP) - Universidad Nacional de La Platafalse
dc.title.none.fl_str_mv On the line shift and oscillator strength of Xe II lines in the spectra of HnMn stars
title On the line shift and oscillator strength of Xe II lines in the spectra of HnMn stars
spellingShingle On the line shift and oscillator strength of Xe II lines in the spectra of HnMn stars
Di Rocco, Héctor O.
Ciencias Astronómicas
Atomic data
Line: identification
Stars: abundances
Stars: chemically peculiar
title_short On the line shift and oscillator strength of Xe II lines in the spectra of HnMn stars
title_full On the line shift and oscillator strength of Xe II lines in the spectra of HnMn stars
title_fullStr On the line shift and oscillator strength of Xe II lines in the spectra of HnMn stars
title_full_unstemmed On the line shift and oscillator strength of Xe II lines in the spectra of HnMn stars
title_sort On the line shift and oscillator strength of Xe II lines in the spectra of HnMn stars
dc.creator.none.fl_str_mv Di Rocco, Héctor O.
Cruzado, Alicia
Marchiano, Paula Esther
author Di Rocco, Héctor O.
author_facet Di Rocco, Héctor O.
Cruzado, Alicia
Marchiano, Paula Esther
author_role author
author2 Cruzado, Alicia
Marchiano, Paula Esther
author2_role author
author
dc.subject.none.fl_str_mv Ciencias Astronómicas
Atomic data
Line: identification
Stars: abundances
Stars: chemically peculiar
topic Ciencias Astronómicas
Atomic data
Line: identification
Stars: abundances
Stars: chemically peculiar
dc.description.none.fl_txt_mv Aims. The ultimate goal that has motivated this work is to achieve realistic oscillator strength (<i>gf</i>) values to find reliable values of stellar abundances. We aim to compare the <i>gf</i> valúes of Xe ii lines found with different theoretical and experimental methods. Methods. We have undertaken calculations using the quasirelativistic and relativistic Hartree-Fock methods. Then we compare these results with those previously obtained from UVES spectra of HgMn stars. Results. 1) Our theoretical <i>gf</i> values are more realistic than those previously obtained for most lines. When we consider only unblended, isolated, relatively noise-free lines, however, our theoretical <i>gf</i> values and Yuce's stellar values differ little from each other. 2) In a discussion of the origin of the previously observed discrepancy between the wavelengths of Xe ii lines deducted from stellar spectra and those published by National Institute of Standards and Technology (NIST), we conclude that stellar wavelengths could be considered the standard wavelengths whenever the densities in stellar atmospheres are smaller than 1 × 10<SUP>16</SUP> part. cm<SUP>-3</SUP>.
Facultad de Ciencias Astronómicas y Geofísicas
Instituto de Astrofísica de La Plata
description Aims. The ultimate goal that has motivated this work is to achieve realistic oscillator strength (<i>gf</i>) values to find reliable values of stellar abundances. We aim to compare the <i>gf</i> valúes of Xe ii lines found with different theoretical and experimental methods. Methods. We have undertaken calculations using the quasirelativistic and relativistic Hartree-Fock methods. Then we compare these results with those previously obtained from UVES spectra of HgMn stars. Results. 1) Our theoretical <i>gf</i> values are more realistic than those previously obtained for most lines. When we consider only unblended, isolated, relatively noise-free lines, however, our theoretical <i>gf</i> values and Yuce's stellar values differ little from each other. 2) In a discussion of the origin of the previously observed discrepancy between the wavelengths of Xe ii lines deducted from stellar spectra and those published by National Institute of Standards and Technology (NIST), we conclude that stellar wavelengths could be considered the standard wavelengths whenever the densities in stellar atmospheres are smaller than 1 × 10<SUP>16</SUP> part. cm<SUP>-3</SUP>.
publishDate 2015
dc.date.none.fl_str_mv 2015
dc.type.none.fl_str_mv info:eu-repo/semantics/article
info:eu-repo/semantics/publishedVersion
Articulo
http://purl.org/coar/resource_type/c_6501
info:ar-repo/semantics/articulo
format article
status_str publishedVersion
dc.identifier.none.fl_str_mv http://sedici.unlp.edu.ar/handle/10915/86392
url http://sedici.unlp.edu.ar/handle/10915/86392
dc.language.none.fl_str_mv eng
language eng
dc.relation.none.fl_str_mv info:eu-repo/semantics/altIdentifier/issn/0004-6361
info:eu-repo/semantics/altIdentifier/doi/10.1051/0004-6361/201526301
dc.rights.none.fl_str_mv info:eu-repo/semantics/openAccess
http://creativecommons.org/licenses/by-nc-sa/4.0/
Creative Commons Attribution-NonCommercial-ShareAlike 4.0 International (CC BY-NC-SA 4.0)
eu_rights_str_mv openAccess
rights_invalid_str_mv http://creativecommons.org/licenses/by-nc-sa/4.0/
Creative Commons Attribution-NonCommercial-ShareAlike 4.0 International (CC BY-NC-SA 4.0)
dc.format.none.fl_str_mv application/pdf
dc.source.none.fl_str_mv reponame:SEDICI (UNLP)
instname:Universidad Nacional de La Plata
instacron:UNLP
reponame_str SEDICI (UNLP)
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instname_str Universidad Nacional de La Plata
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institution UNLP
repository.name.fl_str_mv SEDICI (UNLP) - Universidad Nacional de La Plata
repository.mail.fl_str_mv alira@sedici.unlp.edu.ar
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