High-precision analysis of binary stars with planets. I. Searching for condensation temperature trends in the HD 106515 system

Autores
Saffe, Carlos; Jofre, Jorge Emiliano; Miquelarena Hollger, Paula Andrea; Jaque Arancibia, Marcelo Daniel; Flores Trivigno, Matias Gaston; López, Fernando Marcelo; Collado, Ana Elisa
Año de publicación
2019
Idioma
inglés
Tipo de recurso
artículo
Estado
versión publicada
Descripción
Aims. We explore for the first time the probable chemical signature of planet formation in the remarkable binary system HD 106515. Star A hosts a massive long-period planet with ∼9 MJup detected by radial velocity, while there is no planet detected at the B star. We also refine stellar and planetary parameters by using non-solar-scaled opacities when modelling the stars. Methods. We carried out a simultaneous determination of stellar parameters and abundances by applying for the first time non-solar-scaled opacities in this binary system, in order to reach the highest possible precision. We used a line-by-line strictly differential approach, using the Sun and then the A star as reference. Stellar parameters were determined by imposing an ionization and excitation balance of Fe lines, with an updated version of the FUNDPAR program, ATLAS12 model atmospheres, and the MOOG code. Opacities
for an arbitrary composition were calculated through the opacity sampling method. The chemical patterns were compared with solar-
twins condensation temperature Tc trends from the literature and also mutually between both stars. We take the opportunity to compare
and discuss the results of the classical solar-scaled method and the high-precision procedure applied here. Results. Stars A and B in the binary system HD 106515 do not seem to be depleted in refractory elements, which is different when comparing the Sun with solar twins. The terrestrial planet formation would have been less efficient in the stars of this binary system. Together with HD 80606/7, this is the second binary system that does not seem to present a (terrestrial) signature of planet formation, when both systems host an eccentric giant planet. This is in agreement with numerical simulations, where the early dynamical evolution of eccentric giant planets clears out most of the possible terrestrial planets in the inner zone. We refined the stellar mass, radius, and age for both stars and found a notable difference of ∼78% in R compared to previous works. We also refined the planet mass to mp sin i = 9.08 ± 0.20 MJup, which differs by ∼6% compared with the literature. In addition, we showed that the non-solar-scaled solution is not compatible with the classical solar-scaled method, and some abundance differences are comparable to non-local thermodynamic equilibrium (NLTE) or galactic chemical evolution (GCE) effects especially when using the Sun as reference. Therefore, we encourage the use of non-solar-scaled opacities in high-precision studies such as the detection of Tc trends.


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: Jofre, Jorge Emiliano. Universidad Nacional de Córdoba. Observatorio Astronómico de Córdoba; Argentina. Universidad Nacional Autónoma de México; México. Consejo Nacional de Investigaciones Científicas y Técnicas; Argentina
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: Jaque Arancibia, Marcelo Daniel. Universidad de La Serena; Chile
Fil: Flores Trivigno, Matias Gaston. 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: López, Fernando Marcelo. 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: Collado, Ana Elisa. 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: PLANETARY SYSTEMS
STARS: BINARIES
STARS: INDIVIDUAL: HD 106515
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:11336/124775

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spelling High-precision analysis of binary stars with planets. I. Searching for condensation temperature trends in the HD 106515 systemSaffe, CarlosJofre, Jorge EmilianoMiquelarena Hollger, Paula AndreaJaque Arancibia, Marcelo DanielFlores Trivigno, Matias GastonLópez, Fernando MarceloCollado, Ana ElisaSTARS: ABUNDANCESSTARS: PLANETARY SYSTEMSSTARS: BINARIESSTARS: INDIVIDUAL: HD 106515https://purl.org/becyt/ford/1.3https://purl.org/becyt/ford/1Aims. We explore for the first time the probable chemical signature of planet formation in the remarkable binary system HD 106515. Star A hosts a massive long-period planet with ∼9 MJup detected by radial velocity, while there is no planet detected at the B star. We also refine stellar and planetary parameters by using non-solar-scaled opacities when modelling the stars. Methods. We carried out a simultaneous determination of stellar parameters and abundances by applying for the first time non-solar-scaled opacities in this binary system, in order to reach the highest possible precision. We used a line-by-line strictly differential approach, using the Sun and then the A star as reference. Stellar parameters were determined by imposing an ionization and excitation balance of Fe lines, with an updated version of the FUNDPAR program, ATLAS12 model atmospheres, and the MOOG code. Opacities<br />for an arbitrary composition were calculated through the opacity sampling method. The chemical patterns were compared with solar-<br />twins condensation temperature Tc trends from the literature and also mutually between both stars. We take the opportunity to compare<br /><div>and discuss the results of the classical solar-scaled method and the high-precision procedure applied here. Results. Stars A and B in the binary system HD 106515 do not seem to be depleted in refractory elements, which is different when comparing the Sun with solar twins. The terrestrial planet formation would have been less efficient in the stars of this binary system. Together with HD 80606/7, this is the second binary system that does not seem to present a (terrestrial) signature of planet formation, when both systems host an eccentric giant planet. This is in agreement with numerical simulations, where the early dynamical evolution of eccentric giant planets clears out most of the possible terrestrial planets in the inner zone. We refined the stellar mass, radius, and age for both stars and found a notable difference of ∼78% in R compared to previous works. We also refined the planet mass to mp sin i = 9.08 ± 0.20 MJup, which differs by ∼6% compared with the literature. In addition, we showed that the non-solar-scaled solution is not compatible with the classical solar-scaled method, and some abundance differences are comparable to non-local thermodynamic equilibrium (NLTE) or galactic chemical evolution (GCE) effects especially when using the Sun as reference. Therefore, we encourage the use of non-solar-scaled opacities in high-precision studies such as the detection of Tc trends.</div><div><br /></div>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; ArgentinaFil: Jofre, Jorge Emiliano. Universidad Nacional de Córdoba. Observatorio Astronómico de Córdoba; Argentina. Universidad Nacional Autónoma de México; México. Consejo Nacional de Investigaciones Científicas y Técnicas; ArgentinaFil: 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: Jaque Arancibia, Marcelo Daniel. Universidad de La Serena; ChileFil: Flores Trivigno, Matias Gaston. 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: López, Fernando Marcelo. 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: Collado, Ana Elisa. 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; ArgentinaEDP Sciences2019-04info:eu-repo/semantics/articleinfo:eu-repo/semantics/publishedVersionhttp://purl.org/coar/resource_type/c_6501info:ar-repo/semantics/articuloapplication/pdfapplication/pdfapplication/pdfapplication/pdfapplication/pdfapplication/pdfhttp://hdl.handle.net/11336/124775Saffe, Carlos; Jofre, Jorge Emiliano; Miquelarena Hollger, Paula Andrea; Jaque Arancibia, Marcelo Daniel; Flores Trivigno, Matias Gaston; et al.; High-precision analysis of binary stars with planets. I. Searching for condensation temperature trends in the HD 106515 system; EDP Sciences; Astronomy and Astrophysics; 625; 4-2019; 1-90004-6361CONICET DigitalCONICETenginfo:eu-repo/semantics/altIdentifier/url/https://www.aanda.org/10.1051/0004-6361/201935352info:eu-repo/semantics/altIdentifier/doi/10.1051/0004-6361/201935352info:eu-repo/semantics/openAccesshttps://creativecommons.org/licenses/by-nc-sa/2.5/ar/reponame:CONICET Digital (CONICET)instname:Consejo Nacional de Investigaciones Científicas y Técnicas2025-09-29T10:46:23Zoai:ri.conicet.gov.ar:11336/124775instacron: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 10:46:24.07CONICET Digital (CONICET) - Consejo Nacional de Investigaciones Científicas y Técnicasfalse
dc.title.none.fl_str_mv High-precision analysis of binary stars with planets. I. Searching for condensation temperature trends in the HD 106515 system
title High-precision analysis of binary stars with planets. I. Searching for condensation temperature trends in the HD 106515 system
spellingShingle High-precision analysis of binary stars with planets. I. Searching for condensation temperature trends in the HD 106515 system
Saffe, Carlos
STARS: ABUNDANCES
STARS: PLANETARY SYSTEMS
STARS: BINARIES
STARS: INDIVIDUAL: HD 106515
title_short High-precision analysis of binary stars with planets. I. Searching for condensation temperature trends in the HD 106515 system
title_full High-precision analysis of binary stars with planets. I. Searching for condensation temperature trends in the HD 106515 system
title_fullStr High-precision analysis of binary stars with planets. I. Searching for condensation temperature trends in the HD 106515 system
title_full_unstemmed High-precision analysis of binary stars with planets. I. Searching for condensation temperature trends in the HD 106515 system
title_sort High-precision analysis of binary stars with planets. I. Searching for condensation temperature trends in the HD 106515 system
dc.creator.none.fl_str_mv Saffe, Carlos
Jofre, Jorge Emiliano
Miquelarena Hollger, Paula Andrea
Jaque Arancibia, Marcelo Daniel
Flores Trivigno, Matias Gaston
López, Fernando Marcelo
Collado, Ana Elisa
author Saffe, Carlos
author_facet Saffe, Carlos
Jofre, Jorge Emiliano
Miquelarena Hollger, Paula Andrea
Jaque Arancibia, Marcelo Daniel
Flores Trivigno, Matias Gaston
López, Fernando Marcelo
Collado, Ana Elisa
author_role author
author2 Jofre, Jorge Emiliano
Miquelarena Hollger, Paula Andrea
Jaque Arancibia, Marcelo Daniel
Flores Trivigno, Matias Gaston
López, Fernando Marcelo
Collado, Ana Elisa
author2_role author
author
author
author
author
author
dc.subject.none.fl_str_mv STARS: ABUNDANCES
STARS: PLANETARY SYSTEMS
STARS: BINARIES
STARS: INDIVIDUAL: HD 106515
topic STARS: ABUNDANCES
STARS: PLANETARY SYSTEMS
STARS: BINARIES
STARS: INDIVIDUAL: HD 106515
purl_subject.fl_str_mv https://purl.org/becyt/ford/1.3
https://purl.org/becyt/ford/1
dc.description.none.fl_txt_mv Aims. We explore for the first time the probable chemical signature of planet formation in the remarkable binary system HD 106515. Star A hosts a massive long-period planet with ∼9 MJup detected by radial velocity, while there is no planet detected at the B star. We also refine stellar and planetary parameters by using non-solar-scaled opacities when modelling the stars. Methods. We carried out a simultaneous determination of stellar parameters and abundances by applying for the first time non-solar-scaled opacities in this binary system, in order to reach the highest possible precision. We used a line-by-line strictly differential approach, using the Sun and then the A star as reference. Stellar parameters were determined by imposing an ionization and excitation balance of Fe lines, with an updated version of the FUNDPAR program, ATLAS12 model atmospheres, and the MOOG code. Opacities<br />for an arbitrary composition were calculated through the opacity sampling method. The chemical patterns were compared with solar-<br />twins condensation temperature Tc trends from the literature and also mutually between both stars. We take the opportunity to compare<br /><div>and discuss the results of the classical solar-scaled method and the high-precision procedure applied here. Results. Stars A and B in the binary system HD 106515 do not seem to be depleted in refractory elements, which is different when comparing the Sun with solar twins. The terrestrial planet formation would have been less efficient in the stars of this binary system. Together with HD 80606/7, this is the second binary system that does not seem to present a (terrestrial) signature of planet formation, when both systems host an eccentric giant planet. This is in agreement with numerical simulations, where the early dynamical evolution of eccentric giant planets clears out most of the possible terrestrial planets in the inner zone. We refined the stellar mass, radius, and age for both stars and found a notable difference of ∼78% in R compared to previous works. We also refined the planet mass to mp sin i = 9.08 ± 0.20 MJup, which differs by ∼6% compared with the literature. In addition, we showed that the non-solar-scaled solution is not compatible with the classical solar-scaled method, and some abundance differences are comparable to non-local thermodynamic equilibrium (NLTE) or galactic chemical evolution (GCE) effects especially when using the Sun as reference. Therefore, we encourage the use of non-solar-scaled opacities in high-precision studies such as the detection of Tc trends.</div><div><br /></div>
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: Jofre, Jorge Emiliano. Universidad Nacional de Córdoba. Observatorio Astronómico de Córdoba; Argentina. Universidad Nacional Autónoma de México; México. Consejo Nacional de Investigaciones Científicas y Técnicas; Argentina
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: Jaque Arancibia, Marcelo Daniel. Universidad de La Serena; Chile
Fil: Flores Trivigno, Matias Gaston. 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: López, Fernando Marcelo. 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: Collado, Ana Elisa. 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 Aims. We explore for the first time the probable chemical signature of planet formation in the remarkable binary system HD 106515. Star A hosts a massive long-period planet with ∼9 MJup detected by radial velocity, while there is no planet detected at the B star. We also refine stellar and planetary parameters by using non-solar-scaled opacities when modelling the stars. Methods. We carried out a simultaneous determination of stellar parameters and abundances by applying for the first time non-solar-scaled opacities in this binary system, in order to reach the highest possible precision. We used a line-by-line strictly differential approach, using the Sun and then the A star as reference. Stellar parameters were determined by imposing an ionization and excitation balance of Fe lines, with an updated version of the FUNDPAR program, ATLAS12 model atmospheres, and the MOOG code. Opacities<br />for an arbitrary composition were calculated through the opacity sampling method. The chemical patterns were compared with solar-<br />twins condensation temperature Tc trends from the literature and also mutually between both stars. We take the opportunity to compare<br /><div>and discuss the results of the classical solar-scaled method and the high-precision procedure applied here. Results. Stars A and B in the binary system HD 106515 do not seem to be depleted in refractory elements, which is different when comparing the Sun with solar twins. The terrestrial planet formation would have been less efficient in the stars of this binary system. Together with HD 80606/7, this is the second binary system that does not seem to present a (terrestrial) signature of planet formation, when both systems host an eccentric giant planet. This is in agreement with numerical simulations, where the early dynamical evolution of eccentric giant planets clears out most of the possible terrestrial planets in the inner zone. We refined the stellar mass, radius, and age for both stars and found a notable difference of ∼78% in R compared to previous works. We also refined the planet mass to mp sin i = 9.08 ± 0.20 MJup, which differs by ∼6% compared with the literature. In addition, we showed that the non-solar-scaled solution is not compatible with the classical solar-scaled method, and some abundance differences are comparable to non-local thermodynamic equilibrium (NLTE) or galactic chemical evolution (GCE) effects especially when using the Sun as reference. Therefore, we encourage the use of non-solar-scaled opacities in high-precision studies such as the detection of Tc trends.</div><div><br /></div>
publishDate 2019
dc.date.none.fl_str_mv 2019-04
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/11336/124775
Saffe, Carlos; Jofre, Jorge Emiliano; Miquelarena Hollger, Paula Andrea; Jaque Arancibia, Marcelo Daniel; Flores Trivigno, Matias Gaston; et al.; High-precision analysis of binary stars with planets. I. Searching for condensation temperature trends in the HD 106515 system; EDP Sciences; Astronomy and Astrophysics; 625; 4-2019; 1-9
0004-6361
CONICET Digital
CONICET
url http://hdl.handle.net/11336/124775
identifier_str_mv Saffe, Carlos; Jofre, Jorge Emiliano; Miquelarena Hollger, Paula Andrea; Jaque Arancibia, Marcelo Daniel; Flores Trivigno, Matias Gaston; et al.; High-precision analysis of binary stars with planets. I. Searching for condensation temperature trends in the HD 106515 system; EDP Sciences; Astronomy and Astrophysics; 625; 4-2019; 1-9
0004-6361
CONICET Digital
CONICET
dc.language.none.fl_str_mv eng
language eng
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