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 compareand 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
- Institución
- Consejo Nacional de Investigaciones Científicas y Técnicas
- OAI Identificador
- oai:ri.conicet.gov.ar:11336/124775
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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 |
dc.relation.none.fl_str_mv |
info:eu-repo/semantics/altIdentifier/url/https://www.aanda.org/10.1051/0004-6361/201935352 info:eu-repo/semantics/altIdentifier/doi/10.1051/0004-6361/201935352 |
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 |
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) |
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CONICET Digital (CONICET) |
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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 |
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1844614505462497280 |
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13.070432 |