Stellar parameters and chemical abundances of 223 evolved stars with and without planets

Autores
Jofre, Jorge Emiliano; Petrucci, Romina Paola; Saffe, Carlos; Saker, Leila Yamila; Artur de la Villarmois, E.; Chavero, Carolina Andrea; Gomez, Mercedes Nieves; Mauas, Pablo Jacobo David
Año de publicación
2015
Idioma
inglés
Tipo de recurso
artículo
Estado
versión publicada
Descripción
We present fundamental stellar parameters and chemical abundances for a sample of 86 evolved stars with planets and for a control sample of 137 stars without planets. The analysis was based on both high S/N and resolution echelle spectra. The goals of this work are i) to investigate chemical differences between stars with and without planets; ii) to explore potential differences between the properties of the planets around giants and subgiants; and iii) to search for possible correlations between these properties and the chemical abundances of their host stars. In agreement with previous studies, we find that subgiants with planets are, on average, more metal-rich than subgiants without planets by ~ 0.16 dex. The [Fe/H] distribution of giants with planets is centered at slightly subsolar metallicities and there is no metallicity enhancement relative to the [Fe/H] distribution of giants without planets. Furthermore, contrary to recent results, we do not find any clear difference between the metallicity distributions of stars with and without planets for giants with M > 1.5 Msun. With regard to the other chemical elements, the analysis of the [X/Fe] distributions shows differences between giants with and without planets for some elements, particularly V, Co, and Ba. Analyzing the planet properties, some interesting trends might be emerging: i) multi-planet systems around evolved stars show a slight metallicity enhancement compared with single-planet systems; ii) planets with a $lesssim$ 0.5 AU orbit subgiants with [Fe/H] > 0 and giants hosting planets with a $lesssim$ 1 AU have [Fe/H] < 0; iii) higher-mass planets tend to orbit more metal-poor giants with M < 1.5 Msun, whereas planets around subgiants seem to follow the planet-mass metallicity trend observed on dwarf hosts; iv) planets orbiting giants show lower orbital eccentricities than those orbiting subgiants and dwarfs.
Fil: Jofre, Jorge Emiliano. Universidad Nacional de Cordoba. Observatorio Astronomico de Cordoba. Departamento de Astrofisica Estelar; Argentina. Consejo Nacional de Investigaciones Científicas y Técnicas. Centro Científico Tecnológico Córdoba; Argentina
Fil: Petrucci, Romina Paola. Consejo Nacional de Investigaciones Científicas y Técnicas. Oficina de Coordinación Administrativa Ciudad Universitaria. Instituto de Astronomía y Física del Espacio(i); Argentina
Fil: Saffe, Carlos. Consejo Nacional de Investigaciones Cientiâ­ficas y Tecnicas. Centro Cientifico Tecnologico San Juan. Instituto de Ciencias Astronomicas de la Tierra y del Espacio; Argentina
Fil: Saker, Leila Yamila. Universidad Nacional de Cordoba. Observatorio Astronomico de Cordoba. Departamento de Astrofisica Estelar; Argentina
Fil: Artur de la Villarmois, E.. Universidad Nacional de Cordoba. Observatorio Astronomico de Cordoba. Departamento de Astrofisica Estelar; Argentina
Fil: Chavero, Carolina Andrea. Universidad Nacional de Cordoba. Observatorio Astronomico de Cordoba. Departamento de Astrofisica Estelar; Argentina. Consejo Nacional de Investigaciones Científicas y Técnicas. Centro Científico Tecnológico Córdoba; Argentina
Fil: Gomez, Mercedes Nieves. Universidad Nacional de Cordoba. Observatorio Astronomico de Cordoba. Departamento de Astrofisica Estelar; Argentina. Consejo Nacional de Investigaciones Científicas y Técnicas. Centro Científico Tecnológico Córdoba; Argentina
Fil: Mauas, Pablo Jacobo David. Consejo Nacional de Investigaciones Científicas y Técnicas. Oficina de Coordinación Administrativa Ciudad Universitaria. Instituto de Astronomía y Física del Espacio(i); Argentina
Materia
techniques: spectroscopic
stars: abundances
stars: fundamental parameters
planetary systems
Nivel de accesibilidad
acceso abierto
Condiciones de uso
https://creativecommons.org/licenses/by-nc-sa/2.5/ar/
Repositorio
CONICET Digital (CONICET)
Institución
Consejo Nacional de Investigaciones Científicas y Técnicas
OAI Identificador
oai:ri.conicet.gov.ar:11336/7512
Acceder
id CONICETDig_175d25de9e1d39067ebca811679abb68
oai_identifier_str oai:ri.conicet.gov.ar:11336/7512
network_acronym_str CONICETDig
repository_id_str 3498
network_name_str CONICET Digital (CONICET)
spelling Stellar parameters and chemical abundances of 223 evolved stars with and without planetsJofre, Jorge EmilianoPetrucci, Romina PaolaSaffe, CarlosSaker, Leila YamilaArtur de la Villarmois, E.Chavero, Carolina AndreaGomez, Mercedes NievesMauas, Pablo Jacobo Davidtechniques: spectroscopicstars: abundancesstars: fundamental parametersplanetary systemshttps://purl.org/becyt/ford/1.3https://purl.org/becyt/ford/1We present fundamental stellar parameters and chemical abundances for a sample of 86 evolved stars with planets and for a control sample of 137 stars without planets. The analysis was based on both high S/N and resolution echelle spectra. The goals of this work are i) to investigate chemical differences between stars with and without planets; ii) to explore potential differences between the properties of the planets around giants and subgiants; and iii) to search for possible correlations between these properties and the chemical abundances of their host stars. In agreement with previous studies, we find that subgiants with planets are, on average, more metal-rich than subgiants without planets by ~ 0.16 dex. The [Fe/H] distribution of giants with planets is centered at slightly subsolar metallicities and there is no metallicity enhancement relative to the [Fe/H] distribution of giants without planets. Furthermore, contrary to recent results, we do not find any clear difference between the metallicity distributions of stars with and without planets for giants with M > 1.5 Msun. With regard to the other chemical elements, the analysis of the [X/Fe] distributions shows differences between giants with and without planets for some elements, particularly V, Co, and Ba. Analyzing the planet properties, some interesting trends might be emerging: i) multi-planet systems around evolved stars show a slight metallicity enhancement compared with single-planet systems; ii) planets with a $lesssim$ 0.5 AU orbit subgiants with [Fe/H] > 0 and giants hosting planets with a $lesssim$ 1 AU have [Fe/H] < 0; iii) higher-mass planets tend to orbit more metal-poor giants with M < 1.5 Msun, whereas planets around subgiants seem to follow the planet-mass metallicity trend observed on dwarf hosts; iv) planets orbiting giants show lower orbital eccentricities than those orbiting subgiants and dwarfs.Fil: Jofre, Jorge Emiliano. Universidad Nacional de Cordoba. Observatorio Astronomico de Cordoba. Departamento de Astrofisica Estelar; Argentina. Consejo Nacional de Investigaciones Científicas y Técnicas. Centro Científico Tecnológico Córdoba; ArgentinaFil: Petrucci, Romina Paola. Consejo Nacional de Investigaciones Científicas y Técnicas. Oficina de Coordinación Administrativa Ciudad Universitaria. Instituto de Astronomía y Física del Espacio(i); ArgentinaFil: Saffe, Carlos. Consejo Nacional de Investigaciones Cientiâ­ficas y Tecnicas. Centro Cientifico Tecnologico San Juan. Instituto de Ciencias Astronomicas de la Tierra y del Espacio; ArgentinaFil: Saker, Leila Yamila. Universidad Nacional de Cordoba. Observatorio Astronomico de Cordoba. Departamento de Astrofisica Estelar; ArgentinaFil: Artur de la Villarmois, E.. Universidad Nacional de Cordoba. Observatorio Astronomico de Cordoba. Departamento de Astrofisica Estelar; ArgentinaFil: Chavero, Carolina Andrea. Universidad Nacional de Cordoba. Observatorio Astronomico de Cordoba. Departamento de Astrofisica Estelar; Argentina. Consejo Nacional de Investigaciones Científicas y Técnicas. Centro Científico Tecnológico Córdoba; ArgentinaFil: Gomez, Mercedes Nieves. Universidad Nacional de Cordoba. Observatorio Astronomico de Cordoba. Departamento de Astrofisica Estelar; Argentina. Consejo Nacional de Investigaciones Científicas y Técnicas. Centro Científico Tecnológico Córdoba; ArgentinaFil: Mauas, Pablo Jacobo David. Consejo Nacional de Investigaciones Científicas y Técnicas. Oficina de Coordinación Administrativa Ciudad Universitaria. Instituto de Astronomía y Física del Espacio(i); ArgentinaEdp Sciences2015-02info:eu-repo/semantics/articleinfo:eu-repo/semantics/publishedVersionhttp://purl.org/coar/resource_type/c_6501info:ar-repo/semantics/articuloapplication/pdfapplication/pdfapplication/pdfapplication/pdfapplication/pdfapplication/pdfapplication/pdfhttp://hdl.handle.net/11336/7512Jofre, Jorge Emiliano; Petrucci, Romina Paola; Saffe, Carlos; Saker, Leila Yamila; Artur de la Villarmois, E.; et al.; Stellar parameters and chemical abundances of 223 evolved stars with and without planets; Edp Sciences; Astronomy And Astrophysics; 574; A50; 2-2015; 50-960004-6361enginfo:eu-repo/semantics/altIdentifier/url/http://www.aanda.org/articles/aa/abs/2015/02/aa24474-14/aa24474-14.htmlinfo:eu-repo/semantics/altIdentifier/doi/10.1051/0004-6361/201424474info:eu-repo/semantics/openAccesshttps://creativecommons.org/licenses/by-nc-sa/2.5/ar/reponame:CONICET Digital (CONICET)instname:Consejo Nacional de Investigaciones Científicas y Técnicas2025-09-29T09:52:25Zoai:ri.conicet.gov.ar:11336/7512instacron:CONICETInstitucionalhttp://ri.conicet.gov.ar/Organismo científico-tecnológicoNo correspondehttp://ri.conicet.gov.ar/oai/requestdasensio@conicet.gov.ar; lcarlino@conicet.gov.arArgentinaNo correspondeNo correspondeNo correspondeopendoar:34982025-09-29 09:52:25.671CONICET Digital (CONICET) - Consejo Nacional de Investigaciones Científicas y Técnicasfalse
dc.title.none.fl_str_mv Stellar parameters and chemical abundances of 223 evolved stars with and without planets
title Stellar parameters and chemical abundances of 223 evolved stars with and without planets
spellingShingle Stellar parameters and chemical abundances of 223 evolved stars with and without planets
Jofre, Jorge Emiliano
techniques: spectroscopic
stars: abundances
stars: fundamental parameters
planetary systems
title_short Stellar parameters and chemical abundances of 223 evolved stars with and without planets
title_full Stellar parameters and chemical abundances of 223 evolved stars with and without planets
title_fullStr Stellar parameters and chemical abundances of 223 evolved stars with and without planets
title_full_unstemmed Stellar parameters and chemical abundances of 223 evolved stars with and without planets
title_sort Stellar parameters and chemical abundances of 223 evolved stars with and without planets
dc.creator.none.fl_str_mv Jofre, Jorge Emiliano
Petrucci, Romina Paola
Saffe, Carlos
Saker, Leila Yamila
Artur de la Villarmois, E.
Chavero, Carolina Andrea
Gomez, Mercedes Nieves
Mauas, Pablo Jacobo David
author Jofre, Jorge Emiliano
author_facet Jofre, Jorge Emiliano
Petrucci, Romina Paola
Saffe, Carlos
Saker, Leila Yamila
Artur de la Villarmois, E.
Chavero, Carolina Andrea
Gomez, Mercedes Nieves
Mauas, Pablo Jacobo David
author_role author
author2 Petrucci, Romina Paola
Saffe, Carlos
Saker, Leila Yamila
Artur de la Villarmois, E.
Chavero, Carolina Andrea
Gomez, Mercedes Nieves
Mauas, Pablo Jacobo David
author2_role author
author
author
author
author
author
author
dc.subject.none.fl_str_mv techniques: spectroscopic
stars: abundances
stars: fundamental parameters
planetary systems
topic techniques: spectroscopic
stars: abundances
stars: fundamental parameters
planetary systems
purl_subject.fl_str_mv https://purl.org/becyt/ford/1.3
https://purl.org/becyt/ford/1
dc.description.none.fl_txt_mv We present fundamental stellar parameters and chemical abundances for a sample of 86 evolved stars with planets and for a control sample of 137 stars without planets. The analysis was based on both high S/N and resolution echelle spectra. The goals of this work are i) to investigate chemical differences between stars with and without planets; ii) to explore potential differences between the properties of the planets around giants and subgiants; and iii) to search for possible correlations between these properties and the chemical abundances of their host stars. In agreement with previous studies, we find that subgiants with planets are, on average, more metal-rich than subgiants without planets by ~ 0.16 dex. The [Fe/H] distribution of giants with planets is centered at slightly subsolar metallicities and there is no metallicity enhancement relative to the [Fe/H] distribution of giants without planets. Furthermore, contrary to recent results, we do not find any clear difference between the metallicity distributions of stars with and without planets for giants with M > 1.5 Msun. With regard to the other chemical elements, the analysis of the [X/Fe] distributions shows differences between giants with and without planets for some elements, particularly V, Co, and Ba. Analyzing the planet properties, some interesting trends might be emerging: i) multi-planet systems around evolved stars show a slight metallicity enhancement compared with single-planet systems; ii) planets with a $lesssim$ 0.5 AU orbit subgiants with [Fe/H] > 0 and giants hosting planets with a $lesssim$ 1 AU have [Fe/H] < 0; iii) higher-mass planets tend to orbit more metal-poor giants with M < 1.5 Msun, whereas planets around subgiants seem to follow the planet-mass metallicity trend observed on dwarf hosts; iv) planets orbiting giants show lower orbital eccentricities than those orbiting subgiants and dwarfs.
Fil: Jofre, Jorge Emiliano. Universidad Nacional de Cordoba. Observatorio Astronomico de Cordoba. Departamento de Astrofisica Estelar; Argentina. Consejo Nacional de Investigaciones Científicas y Técnicas. Centro Científico Tecnológico Córdoba; Argentina
Fil: Petrucci, Romina Paola. Consejo Nacional de Investigaciones Científicas y Técnicas. Oficina de Coordinación Administrativa Ciudad Universitaria. Instituto de Astronomía y Física del Espacio(i); Argentina
Fil: Saffe, Carlos. Consejo Nacional de Investigaciones Cientiâ­ficas y Tecnicas. Centro Cientifico Tecnologico San Juan. Instituto de Ciencias Astronomicas de la Tierra y del Espacio; Argentina
Fil: Saker, Leila Yamila. Universidad Nacional de Cordoba. Observatorio Astronomico de Cordoba. Departamento de Astrofisica Estelar; Argentina
Fil: Artur de la Villarmois, E.. Universidad Nacional de Cordoba. Observatorio Astronomico de Cordoba. Departamento de Astrofisica Estelar; Argentina
Fil: Chavero, Carolina Andrea. Universidad Nacional de Cordoba. Observatorio Astronomico de Cordoba. Departamento de Astrofisica Estelar; Argentina. Consejo Nacional de Investigaciones Científicas y Técnicas. Centro Científico Tecnológico Córdoba; Argentina
Fil: Gomez, Mercedes Nieves. Universidad Nacional de Cordoba. Observatorio Astronomico de Cordoba. Departamento de Astrofisica Estelar; Argentina. Consejo Nacional de Investigaciones Científicas y Técnicas. Centro Científico Tecnológico Córdoba; Argentina
Fil: Mauas, Pablo Jacobo David. Consejo Nacional de Investigaciones Científicas y Técnicas. Oficina de Coordinación Administrativa Ciudad Universitaria. Instituto de Astronomía y Física del Espacio(i); Argentina
description We present fundamental stellar parameters and chemical abundances for a sample of 86 evolved stars with planets and for a control sample of 137 stars without planets. The analysis was based on both high S/N and resolution echelle spectra. The goals of this work are i) to investigate chemical differences between stars with and without planets; ii) to explore potential differences between the properties of the planets around giants and subgiants; and iii) to search for possible correlations between these properties and the chemical abundances of their host stars. In agreement with previous studies, we find that subgiants with planets are, on average, more metal-rich than subgiants without planets by ~ 0.16 dex. The [Fe/H] distribution of giants with planets is centered at slightly subsolar metallicities and there is no metallicity enhancement relative to the [Fe/H] distribution of giants without planets. Furthermore, contrary to recent results, we do not find any clear difference between the metallicity distributions of stars with and without planets for giants with M > 1.5 Msun. With regard to the other chemical elements, the analysis of the [X/Fe] distributions shows differences between giants with and without planets for some elements, particularly V, Co, and Ba. Analyzing the planet properties, some interesting trends might be emerging: i) multi-planet systems around evolved stars show a slight metallicity enhancement compared with single-planet systems; ii) planets with a $lesssim$ 0.5 AU orbit subgiants with [Fe/H] > 0 and giants hosting planets with a $lesssim$ 1 AU have [Fe/H] < 0; iii) higher-mass planets tend to orbit more metal-poor giants with M < 1.5 Msun, whereas planets around subgiants seem to follow the planet-mass metallicity trend observed on dwarf hosts; iv) planets orbiting giants show lower orbital eccentricities than those orbiting subgiants and dwarfs.
publishDate 2015
dc.date.none.fl_str_mv 2015-02
dc.type.none.fl_str_mv info:eu-repo/semantics/article
info:eu-repo/semantics/publishedVersion
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://hdl.handle.net/11336/7512
Jofre, Jorge Emiliano; Petrucci, Romina Paola; Saffe, Carlos; Saker, Leila Yamila; Artur de la Villarmois, E.; et al.; Stellar parameters and chemical abundances of 223 evolved stars with and without planets; Edp Sciences; Astronomy And Astrophysics; 574; A50; 2-2015; 50-96
0004-6361
url http://hdl.handle.net/11336/7512
identifier_str_mv Jofre, Jorge Emiliano; Petrucci, Romina Paola; Saffe, Carlos; Saker, Leila Yamila; Artur de la Villarmois, E.; et al.; Stellar parameters and chemical abundances of 223 evolved stars with and without planets; Edp Sciences; Astronomy And Astrophysics; 574; A50; 2-2015; 50-96
0004-6361
dc.language.none.fl_str_mv eng
language eng
dc.relation.none.fl_str_mv info:eu-repo/semantics/altIdentifier/url/http://www.aanda.org/articles/aa/abs/2015/02/aa24474-14/aa24474-14.html
info:eu-repo/semantics/altIdentifier/doi/10.1051/0004-6361/201424474
dc.rights.none.fl_str_mv info:eu-repo/semantics/openAccess
https://creativecommons.org/licenses/by-nc-sa/2.5/ar/
eu_rights_str_mv openAccess
rights_invalid_str_mv https://creativecommons.org/licenses/by-nc-sa/2.5/ar/
dc.format.none.fl_str_mv application/pdf
application/pdf
application/pdf
application/pdf
application/pdf
application/pdf
application/pdf
dc.publisher.none.fl_str_mv Edp Sciences
publisher.none.fl_str_mv Edp Sciences
dc.source.none.fl_str_mv reponame:CONICET Digital (CONICET)
instname:Consejo Nacional de Investigaciones Científicas y Técnicas
reponame_str CONICET Digital (CONICET)
collection CONICET Digital (CONICET)
instname_str Consejo Nacional de Investigaciones Científicas y Técnicas
repository.name.fl_str_mv CONICET Digital (CONICET) - Consejo Nacional de Investigaciones Científicas y Técnicas
repository.mail.fl_str_mv dasensio@conicet.gov.ar; lcarlino@conicet.gov.ar
_version_ 1844613608240054272
score 13.070432

Publicaciones similares