HD 80606: Searching for the chemical signature of planet formation

Context. Binary systems with similar components are ideal laboratories that allow several physical processes to be tested, such as the possible chemical pattern imprinted by the planet formation process. Aims. We explore the probable chemical signature of planet formation in the remarkable binary sy...

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Autor principal:	Buccino, Andrea Paola
Publicado:	2015
Materias:	binaries: general planetary systems stars: abundances stars: individual: HD 80606 Aluminum Bins Planets Refractory materials Systems (metallurgical) Binaries: general Condensation temperature Differential approach Local thermodynamic equilibrium Planetary system Stars: abundances Stars: individual Terrestrial planets Stars
Acceso en línea:	https://bibliotecadigital.exactas.uba.ar/collection/paper/document/paper_00046361_v582_n_p_Saffe http://hdl.handle.net/20.500.12110/paper_00046361_v582_n_p_Saffe
Aporte de:	Biblioteca Digital - Facultad de Ciencias Exactas y Naturales (UBA) de Universidad de Buenos Aires

id	paper:paper_00046361_v582_n_p_Saffe
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spelling	paper:paper_00046361_v582_n_p_Saffe2023-06-08T14:28:11Z HD 80606: Searching for the chemical signature of planet formation Buccino, Andrea Paola binaries: general planetary systems stars: abundances stars: individual: HD 80606 Aluminum Bins Planets Refractory materials Systems (metallurgical) Binaries: general Condensation temperature Differential approach Local thermodynamic equilibrium Planetary system Stars: abundances Stars: individual Terrestrial planets Stars Context. Binary systems with similar components are ideal laboratories that allow several physical processes to be tested, such as the possible chemical pattern imprinted by the planet formation process. Aims. We explore the probable chemical signature of planet formation in the remarkable binary system HD 80606-HD 80607. The star HD80606 hosts a giant planet with ∼4 M<inf>Jup</inf> detected by both transit and radial velocity techniques, which is one of the most eccentric planets detected to date. We study condensation temperature T<inf>c</inf> trends of volatile and refractory element abundances to determine whether there is a depletion of refractories, which could be related to the terrestrial planet formation. Methods. We carried out a high-precision abundance determination in both components of the binary system via a line-by-line, strictly differential approach. First, we used the Sun as a reference and then we used HD80606. The stellar parameters T<inf>eff</inf>, log g, [Fe/H] and v<inf>turb</inf> were determined by imposing differential ionization and excitation equilibrium of Fe I and Fe II lines, with an updated version of the program FUNDPAR, together with plane-parallel local thermodynamic equilibrium (LTE) ATLAS9 model atmospheres and the MOOG code. Then, we derived detailed abundances of 24 different species with equivalent widths and spectral synthesis with the program MOOG. The chemical patterns were compared with the solar-twins T<inf>c</inf> trends of Meléndez et al. (2009, AJ, 704, L66) and with a sample of solar-analogue stars with [Fe/H] ∼ +0.2 dex from Neves et al. (2009, A&A, 497, 563). The T<inf>c</inf> trends were also compared mutually between both stars of the binary system. Results. From the study of T<inf>c</inf> trends, we concluded that the stars HD80606 and HD80607 do not seem to be depleted in refractory elements, which is different for the case of the Sun. Then, following the interpretation of Meléndez et al. (2009), the terrestrial planet formation would have been less efficient in the components of this binary system than in the Sun. The lack of a trend in refractory elements with T<inf>c</inf> between both stars implies that the presence of a giant planet do not neccesarily imprint a chemical signature in their host stars, similar to the recent result of Liu et al. (2014, MNRAS, 442, L51). This is also in agreement with Meléndez et al. (2009), who suggest that the presence of close-in giant planets might prevent the formation of terrestrial planets. Finally, we speculate about a possible, ejected or non-detected, planet around the star HD80607. © ESO, 2015. Fil:Buccino, A. Universidad de Buenos Aires. Facultad de Ciencias Exactas y Naturales; Argentina. 2015 https://bibliotecadigital.exactas.uba.ar/collection/paper/document/paper_00046361_v582_n_p_Saffe http://hdl.handle.net/20.500.12110/paper_00046361_v582_n_p_Saffe
institution	Universidad de Buenos Aires
institution_str	I-28
repository_str	R-134
collection	Biblioteca Digital - Facultad de Ciencias Exactas y Naturales (UBA)
topic	binaries: general planetary systems stars: abundances stars: individual: HD 80606 Aluminum Bins Planets Refractory materials Systems (metallurgical) Binaries: general Condensation temperature Differential approach Local thermodynamic equilibrium Planetary system Stars: abundances Stars: individual Terrestrial planets Stars
spellingShingle	binaries: general planetary systems stars: abundances stars: individual: HD 80606 Aluminum Bins Planets Refractory materials Systems (metallurgical) Binaries: general Condensation temperature Differential approach Local thermodynamic equilibrium Planetary system Stars: abundances Stars: individual Terrestrial planets Stars Buccino, Andrea Paola HD 80606: Searching for the chemical signature of planet formation
topic_facet	binaries: general planetary systems stars: abundances stars: individual: HD 80606 Aluminum Bins Planets Refractory materials Systems (metallurgical) Binaries: general Condensation temperature Differential approach Local thermodynamic equilibrium Planetary system Stars: abundances Stars: individual Terrestrial planets Stars
description	Context. Binary systems with similar components are ideal laboratories that allow several physical processes to be tested, such as the possible chemical pattern imprinted by the planet formation process. Aims. We explore the probable chemical signature of planet formation in the remarkable binary system HD 80606-HD 80607. The star HD80606 hosts a giant planet with ∼4 M<inf>Jup</inf> detected by both transit and radial velocity techniques, which is one of the most eccentric planets detected to date. We study condensation temperature T<inf>c</inf> trends of volatile and refractory element abundances to determine whether there is a depletion of refractories, which could be related to the terrestrial planet formation. Methods. We carried out a high-precision abundance determination in both components of the binary system via a line-by-line, strictly differential approach. First, we used the Sun as a reference and then we used HD80606. The stellar parameters T<inf>eff</inf>, log g, [Fe/H] and v<inf>turb</inf> were determined by imposing differential ionization and excitation equilibrium of Fe I and Fe II lines, with an updated version of the program FUNDPAR, together with plane-parallel local thermodynamic equilibrium (LTE) ATLAS9 model atmospheres and the MOOG code. Then, we derived detailed abundances of 24 different species with equivalent widths and spectral synthesis with the program MOOG. The chemical patterns were compared with the solar-twins T<inf>c</inf> trends of Meléndez et al. (2009, AJ, 704, L66) and with a sample of solar-analogue stars with [Fe/H] ∼ +0.2 dex from Neves et al. (2009, A&A, 497, 563). The T<inf>c</inf> trends were also compared mutually between both stars of the binary system. Results. From the study of T<inf>c</inf> trends, we concluded that the stars HD80606 and HD80607 do not seem to be depleted in refractory elements, which is different for the case of the Sun. Then, following the interpretation of Meléndez et al. (2009), the terrestrial planet formation would have been less efficient in the components of this binary system than in the Sun. The lack of a trend in refractory elements with T<inf>c</inf> between both stars implies that the presence of a giant planet do not neccesarily imprint a chemical signature in their host stars, similar to the recent result of Liu et al. (2014, MNRAS, 442, L51). This is also in agreement with Meléndez et al. (2009), who suggest that the presence of close-in giant planets might prevent the formation of terrestrial planets. Finally, we speculate about a possible, ejected or non-detected, planet around the star HD80607. © ESO, 2015.
author	Buccino, Andrea Paola
author_facet	Buccino, Andrea Paola
author_sort	Buccino, Andrea Paola
title	HD 80606: Searching for the chemical signature of planet formation
title_short	HD 80606: Searching for the chemical signature of planet formation
title_full	HD 80606: Searching for the chemical signature of planet formation
title_fullStr	HD 80606: Searching for the chemical signature of planet formation
title_full_unstemmed	HD 80606: Searching for the chemical signature of planet formation
title_sort	hd 80606: searching for the chemical signature of planet formation
publishDate	2015
url	https://bibliotecadigital.exactas.uba.ar/collection/paper/document/paper_00046361_v582_n_p_Saffe http://hdl.handle.net/20.500.12110/paper_00046361_v582_n_p_Saffe
work_keys_str_mv	AT buccinoandreapaola hd80606searchingforthechemicalsignatureofplanetformation
_version_	1768546701729071104

HD 80606: Searching for the chemical signature of planet formation

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