Elemental abundances differences in the massive planet-hosting wide binary HD 196067-68
- Autores
- Flores, Matias; Galarza, J. Yana; Miquelarena Hollger, Paula Andrea; Saffe, Carlos; Arancibia, M. Jaque; Ibañez Bustos, Romina Valeria; Jofre, Jorge Emiliano; Alacoria, José Alberto; Gunella Toledo, Jose Fernando
- Año de publicación
- 2023
- Idioma
- inglés
- Tipo de recurso
- artículo
- Estado
- versión publicada
- Descripción
- It has been suggested that small chemical anomalies observed in planet-hosting wide binary systems could be due to planet signatures, where the role of the planetary mass is still unknown. We search for a possible planet signature by analyzing the TC trends in the remarkable binary system HD 196067–HD 196068. At the moment, only HD 196067 is known to host a planet which is near the brown dwarf regime. We take advantage of the strong physical similarity between both stars, which is crucial to achieving the highest possible precision in stellar parameters and elemental chemical abundances. This system gives us a unique opportunity to explore if a possible depletion of refractories in a binary system could be inhibited by the presence of a massive planet. We performed a line-by-line chemical differential study, employing the non-solar-scaled opacities, in order to reach the highest precision in the calculations. After differentially comparing both stars, HD 196067 displays a clear deficiency in refractory elements in the TC plane, a lower iron content (0.051 dex) and also a lower Li i content (0.14 dex) than its companion. In addition, the differential abundances reveal a TC trend. These targets represent the first cases of an abundance difference around a binary system hosting a super-Jupiter. Although we explored several scenarios to explain the chemical anomalies, none of them can be entirely ruled out. Additional monitoring of the system as well as studies of larger sample of wide binary systems hosting massive planets, are needed to better understand the chemical abundance trend observed in HD 196067-68.
Fil: Flores, Matias. Consejo Nacional de Investigaciones Científicas y Técnicas. Centro Científico Tecnológico Conicet - San Juan. Instituto de Ciencias Astronómicas, de la Tierra y del Espacio. Universidad Nacional de San Juan. Instituto de Ciencias Astronómicas, de la Tierra y del Espacio; Argentina
Fil: Galarza, J. Yana. Carnegie Observatories; Estados Unidos
Fil: Miquelarena Hollger, Paula Andrea. Consejo Nacional de Investigaciones Científicas y Técnicas. Centro Científico Tecnológico Conicet - San Juan. Instituto de Ciencias Astronómicas, de la Tierra y del Espacio. Universidad Nacional de San Juan. Instituto de Ciencias Astronómicas, de la Tierra y del Espacio; Argentina
Fil: Saffe, Carlos. Consejo Nacional de Investigaciones Científicas y Técnicas. Centro Científico Tecnológico Conicet - San Juan. Instituto de Ciencias Astronómicas, de la Tierra y del Espacio. Universidad Nacional de San Juan. Instituto de Ciencias Astronómicas, de la Tierra y del Espacio; Argentina
Fil: Arancibia, M. Jaque. Universidad de La Serena; Chile
Fil: Ibañez Bustos, Romina Valeria. Observatoire de la Cote D'Azur; Francia. Centre National de la Recherche Scientifique; Francia. Consejo Nacional de Investigaciones Científicas y Técnicas; Argentina
Fil: Jofre, Jorge Emiliano. Universidad Nacional de Córdoba. Observatorio Astronómico de Córdoba; Argentina. Consejo Nacional de Investigaciones Científicas y Técnicas. Centro Científico Tecnológico Conicet - Córdoba; Argentina
Fil: Alacoria, José Alberto. Consejo Nacional de Investigaciones Científicas y Técnicas. Centro Científico Tecnológico Conicet - San Juan. Instituto de Ciencias Astronómicas, de la Tierra y del Espacio. Universidad Nacional de San Juan. Instituto de Ciencias Astronómicas, de la Tierra y del Espacio; Argentina
Fil: Gunella Toledo, Jose Fernando. Consejo Nacional de Investigaciones Científicas y Técnicas. Centro Científico Tecnológico Conicet - San Juan. Instituto de Ciencias Astronómicas, de la Tierra y del Espacio. Universidad Nacional de San Juan. Instituto de Ciencias Astronómicas, de la Tierra y del Espacio; Argentina - Materia
-
STARS: ABUNDANCES
STARS: BINARIES: GENERAL
STARS: FUNDAMENTAL PARAMETERS
STARS: INDIVIDUAL: HD 196067-68 - Nivel de accesibilidad
- acceso abierto
- Condiciones de uso
- https://creativecommons.org/licenses/by-nc-sa/2.5/ar/
- Repositorio
- Institución
- Consejo Nacional de Investigaciones Científicas y Técnicas
- OAI Identificador
- oai:ri.conicet.gov.ar:11336/222630
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Elemental abundances differences in the massive planet-hosting wide binary HD 196067-68Flores, MatiasGalarza, J. YanaMiquelarena Hollger, Paula AndreaSaffe, CarlosArancibia, M. JaqueIbañez Bustos, Romina ValeriaJofre, Jorge EmilianoAlacoria, José AlbertoGunella Toledo, Jose FernandoSTARS: ABUNDANCESSTARS: BINARIES: GENERALSTARS: FUNDAMENTAL PARAMETERSSTARS: INDIVIDUAL: HD 196067-68https://purl.org/becyt/ford/1.3https://purl.org/becyt/ford/1It has been suggested that small chemical anomalies observed in planet-hosting wide binary systems could be due to planet signatures, where the role of the planetary mass is still unknown. We search for a possible planet signature by analyzing the TC trends in the remarkable binary system HD 196067–HD 196068. At the moment, only HD 196067 is known to host a planet which is near the brown dwarf regime. We take advantage of the strong physical similarity between both stars, which is crucial to achieving the highest possible precision in stellar parameters and elemental chemical abundances. This system gives us a unique opportunity to explore if a possible depletion of refractories in a binary system could be inhibited by the presence of a massive planet. We performed a line-by-line chemical differential study, employing the non-solar-scaled opacities, in order to reach the highest precision in the calculations. After differentially comparing both stars, HD 196067 displays a clear deficiency in refractory elements in the TC plane, a lower iron content (0.051 dex) and also a lower Li i content (0.14 dex) than its companion. In addition, the differential abundances reveal a TC trend. These targets represent the first cases of an abundance difference around a binary system hosting a super-Jupiter. Although we explored several scenarios to explain the chemical anomalies, none of them can be entirely ruled out. Additional monitoring of the system as well as studies of larger sample of wide binary systems hosting massive planets, are needed to better understand the chemical abundance trend observed in HD 196067-68.Fil: Flores, Matias. Consejo Nacional de Investigaciones Científicas y Técnicas. Centro Científico Tecnológico Conicet - San Juan. Instituto de Ciencias Astronómicas, de la Tierra y del Espacio. Universidad Nacional de San Juan. Instituto de Ciencias Astronómicas, de la Tierra y del Espacio; ArgentinaFil: Galarza, J. Yana. Carnegie Observatories; Estados UnidosFil: Miquelarena Hollger, Paula Andrea. Consejo Nacional de Investigaciones Científicas y Técnicas. Centro Científico Tecnológico Conicet - San Juan. Instituto de Ciencias Astronómicas, de la Tierra y del Espacio. Universidad Nacional de San Juan. Instituto de Ciencias Astronómicas, de la Tierra y del Espacio; ArgentinaFil: Saffe, Carlos. Consejo Nacional de Investigaciones Científicas y Técnicas. Centro Científico Tecnológico Conicet - San Juan. Instituto de Ciencias Astronómicas, de la Tierra y del Espacio. Universidad Nacional de San Juan. Instituto de Ciencias Astronómicas, de la Tierra y del Espacio; ArgentinaFil: Arancibia, M. Jaque. Universidad de La Serena; ChileFil: Ibañez Bustos, Romina Valeria. Observatoire de la Cote D'Azur; Francia. Centre National de la Recherche Scientifique; Francia. Consejo Nacional de Investigaciones Científicas y Técnicas; ArgentinaFil: Jofre, Jorge Emiliano. Universidad Nacional de Córdoba. Observatorio Astronómico de Córdoba; Argentina. Consejo Nacional de Investigaciones Científicas y Técnicas. Centro Científico Tecnológico Conicet - Córdoba; ArgentinaFil: Alacoria, José Alberto. Consejo Nacional de Investigaciones Científicas y Técnicas. Centro Científico Tecnológico Conicet - San Juan. Instituto de Ciencias Astronómicas, de la Tierra y del Espacio. Universidad Nacional de San Juan. Instituto de Ciencias Astronómicas, de la Tierra y del Espacio; ArgentinaFil: Gunella Toledo, Jose Fernando. Consejo Nacional de Investigaciones Científicas y Técnicas. Centro Científico Tecnológico Conicet - San Juan. Instituto de Ciencias Astronómicas, de la Tierra y del Espacio. Universidad Nacional de San Juan. Instituto de Ciencias Astronómicas, de la Tierra y del Espacio; ArgentinaWiley Blackwell Publishing, Inc2023-12info:eu-repo/semantics/articleinfo:eu-repo/semantics/publishedVersionhttp://purl.org/coar/resource_type/c_6501info:ar-repo/semantics/articuloapplication/pdfapplication/pdfhttp://hdl.handle.net/11336/222630Flores, Matias; Galarza, J. Yana; Miquelarena Hollger, Paula Andrea; Saffe, Carlos; Arancibia, M. Jaque; et al.; Elemental abundances differences in the massive planet-hosting wide binary HD 196067-68; Wiley Blackwell Publishing, Inc; Monthly Notices of the Royal Astronomical Society; 12-20230035-8711CONICET DigitalCONICETenginfo:eu-repo/semantics/altIdentifier/url/https://academic.oup.com/mnras/advance-article/doi/10.1093/mnras/stad3714/7459956info:eu-repo/semantics/altIdentifier/doi/10.1093/mnras/stad3714info:eu-repo/semantics/openAccesshttps://creativecommons.org/licenses/by-nc-sa/2.5/ar/reponame:CONICET Digital (CONICET)instname:Consejo Nacional de Investigaciones Científicas y Técnicas2025-09-29T10:20:20Zoai:ri.conicet.gov.ar:11336/222630instacron: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 10:20:21.21CONICET Digital (CONICET) - Consejo Nacional de Investigaciones Científicas y Técnicasfalse |
dc.title.none.fl_str_mv |
Elemental abundances differences in the massive planet-hosting wide binary HD 196067-68 |
title |
Elemental abundances differences in the massive planet-hosting wide binary HD 196067-68 |
spellingShingle |
Elemental abundances differences in the massive planet-hosting wide binary HD 196067-68 Flores, Matias STARS: ABUNDANCES STARS: BINARIES: GENERAL STARS: FUNDAMENTAL PARAMETERS STARS: INDIVIDUAL: HD 196067-68 |
title_short |
Elemental abundances differences in the massive planet-hosting wide binary HD 196067-68 |
title_full |
Elemental abundances differences in the massive planet-hosting wide binary HD 196067-68 |
title_fullStr |
Elemental abundances differences in the massive planet-hosting wide binary HD 196067-68 |
title_full_unstemmed |
Elemental abundances differences in the massive planet-hosting wide binary HD 196067-68 |
title_sort |
Elemental abundances differences in the massive planet-hosting wide binary HD 196067-68 |
dc.creator.none.fl_str_mv |
Flores, Matias Galarza, J. Yana Miquelarena Hollger, Paula Andrea Saffe, Carlos Arancibia, M. Jaque Ibañez Bustos, Romina Valeria Jofre, Jorge Emiliano Alacoria, José Alberto Gunella Toledo, Jose Fernando |
author |
Flores, Matias |
author_facet |
Flores, Matias Galarza, J. Yana Miquelarena Hollger, Paula Andrea Saffe, Carlos Arancibia, M. Jaque Ibañez Bustos, Romina Valeria Jofre, Jorge Emiliano Alacoria, José Alberto Gunella Toledo, Jose Fernando |
author_role |
author |
author2 |
Galarza, J. Yana Miquelarena Hollger, Paula Andrea Saffe, Carlos Arancibia, M. Jaque Ibañez Bustos, Romina Valeria Jofre, Jorge Emiliano Alacoria, José Alberto Gunella Toledo, Jose Fernando |
author2_role |
author author author author author author author author |
dc.subject.none.fl_str_mv |
STARS: ABUNDANCES STARS: BINARIES: GENERAL STARS: FUNDAMENTAL PARAMETERS STARS: INDIVIDUAL: HD 196067-68 |
topic |
STARS: ABUNDANCES STARS: BINARIES: GENERAL STARS: FUNDAMENTAL PARAMETERS STARS: INDIVIDUAL: HD 196067-68 |
purl_subject.fl_str_mv |
https://purl.org/becyt/ford/1.3 https://purl.org/becyt/ford/1 |
dc.description.none.fl_txt_mv |
It has been suggested that small chemical anomalies observed in planet-hosting wide binary systems could be due to planet signatures, where the role of the planetary mass is still unknown. We search for a possible planet signature by analyzing the TC trends in the remarkable binary system HD 196067–HD 196068. At the moment, only HD 196067 is known to host a planet which is near the brown dwarf regime. We take advantage of the strong physical similarity between both stars, which is crucial to achieving the highest possible precision in stellar parameters and elemental chemical abundances. This system gives us a unique opportunity to explore if a possible depletion of refractories in a binary system could be inhibited by the presence of a massive planet. We performed a line-by-line chemical differential study, employing the non-solar-scaled opacities, in order to reach the highest precision in the calculations. After differentially comparing both stars, HD 196067 displays a clear deficiency in refractory elements in the TC plane, a lower iron content (0.051 dex) and also a lower Li i content (0.14 dex) than its companion. In addition, the differential abundances reveal a TC trend. These targets represent the first cases of an abundance difference around a binary system hosting a super-Jupiter. Although we explored several scenarios to explain the chemical anomalies, none of them can be entirely ruled out. Additional monitoring of the system as well as studies of larger sample of wide binary systems hosting massive planets, are needed to better understand the chemical abundance trend observed in HD 196067-68. Fil: Flores, Matias. Consejo Nacional de Investigaciones Científicas y Técnicas. Centro Científico Tecnológico Conicet - San Juan. Instituto de Ciencias Astronómicas, de la Tierra y del Espacio. Universidad Nacional de San Juan. Instituto de Ciencias Astronómicas, de la Tierra y del Espacio; Argentina Fil: Galarza, J. Yana. Carnegie Observatories; Estados Unidos Fil: Miquelarena Hollger, Paula Andrea. Consejo Nacional de Investigaciones Científicas y Técnicas. Centro Científico Tecnológico Conicet - San Juan. Instituto de Ciencias Astronómicas, de la Tierra y del Espacio. Universidad Nacional de San Juan. Instituto de Ciencias Astronómicas, de la Tierra y del Espacio; Argentina Fil: Saffe, Carlos. Consejo Nacional de Investigaciones Científicas y Técnicas. Centro Científico Tecnológico Conicet - San Juan. Instituto de Ciencias Astronómicas, de la Tierra y del Espacio. Universidad Nacional de San Juan. Instituto de Ciencias Astronómicas, de la Tierra y del Espacio; Argentina Fil: Arancibia, M. Jaque. Universidad de La Serena; Chile Fil: Ibañez Bustos, Romina Valeria. Observatoire de la Cote D'Azur; Francia. Centre National de la Recherche Scientifique; Francia. Consejo Nacional de Investigaciones Científicas y Técnicas; Argentina Fil: Jofre, Jorge Emiliano. Universidad Nacional de Córdoba. Observatorio Astronómico de Córdoba; Argentina. Consejo Nacional de Investigaciones Científicas y Técnicas. Centro Científico Tecnológico Conicet - Córdoba; Argentina Fil: Alacoria, José Alberto. Consejo Nacional de Investigaciones Científicas y Técnicas. Centro Científico Tecnológico Conicet - San Juan. Instituto de Ciencias Astronómicas, de la Tierra y del Espacio. Universidad Nacional de San Juan. Instituto de Ciencias Astronómicas, de la Tierra y del Espacio; Argentina Fil: Gunella Toledo, Jose Fernando. Consejo Nacional de Investigaciones Científicas y Técnicas. Centro Científico Tecnológico Conicet - San Juan. Instituto de Ciencias Astronómicas, de la Tierra y del Espacio. Universidad Nacional de San Juan. Instituto de Ciencias Astronómicas, de la Tierra y del Espacio; Argentina |
description |
It has been suggested that small chemical anomalies observed in planet-hosting wide binary systems could be due to planet signatures, where the role of the planetary mass is still unknown. We search for a possible planet signature by analyzing the TC trends in the remarkable binary system HD 196067–HD 196068. At the moment, only HD 196067 is known to host a planet which is near the brown dwarf regime. We take advantage of the strong physical similarity between both stars, which is crucial to achieving the highest possible precision in stellar parameters and elemental chemical abundances. This system gives us a unique opportunity to explore if a possible depletion of refractories in a binary system could be inhibited by the presence of a massive planet. We performed a line-by-line chemical differential study, employing the non-solar-scaled opacities, in order to reach the highest precision in the calculations. After differentially comparing both stars, HD 196067 displays a clear deficiency in refractory elements in the TC plane, a lower iron content (0.051 dex) and also a lower Li i content (0.14 dex) than its companion. In addition, the differential abundances reveal a TC trend. These targets represent the first cases of an abundance difference around a binary system hosting a super-Jupiter. Although we explored several scenarios to explain the chemical anomalies, none of them can be entirely ruled out. Additional monitoring of the system as well as studies of larger sample of wide binary systems hosting massive planets, are needed to better understand the chemical abundance trend observed in HD 196067-68. |
publishDate |
2023 |
dc.date.none.fl_str_mv |
2023-12 |
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/11336/222630 Flores, Matias; Galarza, J. Yana; Miquelarena Hollger, Paula Andrea; Saffe, Carlos; Arancibia, M. Jaque; et al.; Elemental abundances differences in the massive planet-hosting wide binary HD 196067-68; Wiley Blackwell Publishing, Inc; Monthly Notices of the Royal Astronomical Society; 12-2023 0035-8711 CONICET Digital CONICET |
url |
http://hdl.handle.net/11336/222630 |
identifier_str_mv |
Flores, Matias; Galarza, J. Yana; Miquelarena Hollger, Paula Andrea; Saffe, Carlos; Arancibia, M. Jaque; et al.; Elemental abundances differences in the massive planet-hosting wide binary HD 196067-68; Wiley Blackwell Publishing, Inc; Monthly Notices of the Royal Astronomical Society; 12-2023 0035-8711 CONICET Digital CONICET |
dc.language.none.fl_str_mv |
eng |
language |
eng |
dc.relation.none.fl_str_mv |
info:eu-repo/semantics/altIdentifier/url/https://academic.oup.com/mnras/advance-article/doi/10.1093/mnras/stad3714/7459956 info:eu-repo/semantics/altIdentifier/doi/10.1093/mnras/stad3714 |
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 |
dc.publisher.none.fl_str_mv |
Wiley Blackwell Publishing, Inc |
publisher.none.fl_str_mv |
Wiley Blackwell Publishing, Inc |
dc.source.none.fl_str_mv |
reponame:CONICET Digital (CONICET) instname:Consejo Nacional de Investigaciones Científicas y Técnicas |
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CONICET Digital (CONICET) |
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CONICET Digital (CONICET) |
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Consejo Nacional de Investigaciones Científicas y Técnicas |
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CONICET Digital (CONICET) - Consejo Nacional de Investigaciones Científicas y Técnicas |
repository.mail.fl_str_mv |
dasensio@conicet.gov.ar; lcarlino@conicet.gov.ar |
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1844614183553859584 |
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13.070432 |