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
- Institución
- Universidad Nacional de La Plata
- OAI Identificador
- oai:sedici.unlp.edu.ar:10915/86392
Ver los metadatos del registro completo
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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 |
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SEDICI (UNLP) - Universidad Nacional de La Plata |
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