On the age of the magnetically active WW Psa and TX Psa members of the beta Pictoris association

Autores
Messina, S.; Santallo, R.; Tan, T.; Elliot, P.; Feiden, G.; Buccino, Andrea Paola; Mauas, Pablo Jacobo David; Petrucci, Romina Paola; Jofré, E.
Año de publicación
2016
Idioma
inglés
Tipo de recurso
artículo
Estado
versión publicada
Descripción
Context. There are a variety of different techniques available to estimate the ages of pre-main-sequence stars. Components of physical pairs, thanks to their strict coevality and the mass difference, such as the binary system analyzed in this paper, are best suited to test the effectiveness of these different techniques. Aims. We consider the system WW Psa + TX Psa whose membership of the 25-Myr β Pictoris association has been well established by earlier works. We aim to investigate which age-dating technique provides the best agreement between the age of the system and that of the association. Methods. We have photometrically monitored WW Psa and TX Psa and measured their rotation periods as P = 2.37 d and P = 1.086 d, respectively. We have retrieved their Li equivalent widths from the literature and measured their effective temperatures and luminosities. We investigated whether the ages of these stars derived using three independent techniques, that is based on rotation, Li equivalent widths, and the position in the HR diagram are consistent with the age of the β Pictoris association. Results. We find that the rotation periods and the Li contents of both stars are consistent with the distribution of other bona fide members of the cluster. On the contrary, the isochronal fitting provides similar ages for both stars, but a factor of about four younger than the quoted age of the association, or about 30% younger when the effects of magnetic fields are included. Conclusions. We explore the origin of the discrepant age inferred from isochronal fitting, including the possibilities that either the two components may be unresolved binaries or that the basic stellar parameters of both components are altered by enhanced magnetic activity. The latter is found to be the more reasonable cause, suggesting that age estimates based on Li content are more reliable than isochronal fitting for pre-main-sequence stars with pronounced magnetic activity.
Fil: Messina, S.. Osservatorio Astrofisico Di Catania; Italia
Fil: Santallo, R.. Southern Stars Observatory; Polinesia Francesa
Fil: Tan, T.. Perth Exoplanet Survey Telescope; Australia
Fil: Elliot, P.. European Southern Observatory; Chile
Fil: Feiden, G.. Uppsala Universitet; Suecia
Fil: Buccino, Andrea Paola. Consejo Nacional de Investigaciones Científicas y Técnicas. Oficina de Coordinación Administrativa Ciudad Universitaria. Instituto de Astronomía y Física del Espacio. - Universidad de Buenos Aires. Facultad de Ciencias Exactas y Naturales. Instituto de Astronomía y Física del Espacio; 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. - Universidad de Buenos Aires. Facultad de Ciencias Exactas y Naturales. Instituto de Astronomía y Física del Espacio; Argentina
Fil: Petrucci, Romina Paola. Universidad Nacional de Córdoba. Observatorio Astronómico de Córdoba; Argentina. Consejo Nacional de Investigaciones Científicas y Técnicas. Centro Científico Tecnológico Conicet - Córdoba; Argentina
Fil: Jofré, E.. Universidad Nacional de Córdoba. Observatorio Astronómico de Córdoba; Argentina
Materia
BINARIES: GENERAL
STARS: ACTIVITY
STARS: LATE-TYPE
STARS: LOW-MASS
STARSPOTS
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:11336/180085
Acceder
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oai_identifier_str oai:ri.conicet.gov.ar:11336/180085
network_acronym_str CONICETDig
repository_id_str 3498
network_name_str CONICET Digital (CONICET)
spelling On the age of the magnetically active WW Psa and TX Psa members of the beta Pictoris associationMessina, S.Santallo, R.Tan, T.Elliot, P.Feiden, G.Buccino, Andrea PaolaMauas, Pablo Jacobo DavidPetrucci, Romina PaolaJofré, E.BINARIES: GENERALSTARS: ACTIVITYSTARS: LATE-TYPESTARS: LOW-MASSSTARSPOTShttps://purl.org/becyt/ford/1.7https://purl.org/becyt/ford/1Context. There are a variety of different techniques available to estimate the ages of pre-main-sequence stars. Components of physical pairs, thanks to their strict coevality and the mass difference, such as the binary system analyzed in this paper, are best suited to test the effectiveness of these different techniques. Aims. We consider the system WW Psa + TX Psa whose membership of the 25-Myr β Pictoris association has been well established by earlier works. We aim to investigate which age-dating technique provides the best agreement between the age of the system and that of the association. Methods. We have photometrically monitored WW Psa and TX Psa and measured their rotation periods as P = 2.37 d and P = 1.086 d, respectively. We have retrieved their Li equivalent widths from the literature and measured their effective temperatures and luminosities. We investigated whether the ages of these stars derived using three independent techniques, that is based on rotation, Li equivalent widths, and the position in the HR diagram are consistent with the age of the β Pictoris association. Results. We find that the rotation periods and the Li contents of both stars are consistent with the distribution of other bona fide members of the cluster. On the contrary, the isochronal fitting provides similar ages for both stars, but a factor of about four younger than the quoted age of the association, or about 30% younger when the effects of magnetic fields are included. Conclusions. We explore the origin of the discrepant age inferred from isochronal fitting, including the possibilities that either the two components may be unresolved binaries or that the basic stellar parameters of both components are altered by enhanced magnetic activity. The latter is found to be the more reasonable cause, suggesting that age estimates based on Li content are more reliable than isochronal fitting for pre-main-sequence stars with pronounced magnetic activity.Fil: Messina, S.. Osservatorio Astrofisico Di Catania; ItaliaFil: Santallo, R.. Southern Stars Observatory; Polinesia FrancesaFil: Tan, T.. Perth Exoplanet Survey Telescope; AustraliaFil: Elliot, P.. European Southern Observatory; ChileFil: Feiden, G.. Uppsala Universitet; SueciaFil: Buccino, Andrea Paola. Consejo Nacional de Investigaciones Científicas y Técnicas. Oficina de Coordinación Administrativa Ciudad Universitaria. Instituto de Astronomía y Física del Espacio. - Universidad de Buenos Aires. Facultad de Ciencias Exactas y Naturales. Instituto de Astronomía y Física del Espacio; 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. - Universidad de Buenos Aires. Facultad de Ciencias Exactas y Naturales. Instituto de Astronomía y Física del Espacio; ArgentinaFil: Petrucci, Romina Paola. Universidad Nacional de Córdoba. Observatorio Astronómico de Córdoba; Argentina. Consejo Nacional de Investigaciones Científicas y Técnicas. Centro Científico Tecnológico Conicet - Córdoba; ArgentinaFil: Jofré, E.. Universidad Nacional de Córdoba. Observatorio Astronómico de Córdoba; ArgentinaEDP Sciences2016-12info:eu-repo/semantics/articleinfo:eu-repo/semantics/publishedVersionhttp://purl.org/coar/resource_type/c_6501info:ar-repo/semantics/articuloapplication/pdfapplication/pdfhttp://hdl.handle.net/11336/180085Messina, S.; Santallo, R.; Tan, T.; Elliot, P.; Feiden, G.; et al.; On the age of the magnetically active WW Psa and TX Psa members of the beta Pictoris association; EDP Sciences; Astronomy and Astrophysics; 601; A54; 12-2016; 1-120004-6361CONICET DigitalCONICETenginfo:eu-repo/semantics/altIdentifier/url/https://www.aanda.org/articles/aa/pdf/2017/05/aa28514-16.pdfinfo:eu-repo/semantics/altIdentifier/doi/10.1051/0004-6361/201628514info:eu-repo/semantics/openAccesshttps://creativecommons.org/licenses/by-nc-sa/2.5/ar/reponame:CONICET Digital (CONICET)instname:Consejo Nacional de Investigaciones Científicas y Técnicas2025-10-22T11:15:01Zoai:ri.conicet.gov.ar:11336/180085instacron: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:34982025-10-22 11:15:02.109CONICET Digital (CONICET) - Consejo Nacional de Investigaciones Científicas y Técnicasfalse
dc.title.none.fl_str_mv On the age of the magnetically active WW Psa and TX Psa members of the beta Pictoris association
title On the age of the magnetically active WW Psa and TX Psa members of the beta Pictoris association
spellingShingle On the age of the magnetically active WW Psa and TX Psa members of the beta Pictoris association
Messina, S.
BINARIES: GENERAL
STARS: ACTIVITY
STARS: LATE-TYPE
STARS: LOW-MASS
STARSPOTS
title_short On the age of the magnetically active WW Psa and TX Psa members of the beta Pictoris association
title_full On the age of the magnetically active WW Psa and TX Psa members of the beta Pictoris association
title_fullStr On the age of the magnetically active WW Psa and TX Psa members of the beta Pictoris association
title_full_unstemmed On the age of the magnetically active WW Psa and TX Psa members of the beta Pictoris association
title_sort On the age of the magnetically active WW Psa and TX Psa members of the beta Pictoris association
dc.creator.none.fl_str_mv Messina, S.
Santallo, R.
Tan, T.
Elliot, P.
Feiden, G.
Buccino, Andrea Paola
Mauas, Pablo Jacobo David
Petrucci, Romina Paola
Jofré, E.
author Messina, S.
author_facet Messina, S.
Santallo, R.
Tan, T.
Elliot, P.
Feiden, G.
Buccino, Andrea Paola
Mauas, Pablo Jacobo David
Petrucci, Romina Paola
Jofré, E.
author_role author
author2 Santallo, R.
Tan, T.
Elliot, P.
Feiden, G.
Buccino, Andrea Paola
Mauas, Pablo Jacobo David
Petrucci, Romina Paola
Jofré, E.
author2_role author
author
author
author
author
author
author
author
dc.subject.none.fl_str_mv BINARIES: GENERAL
STARS: ACTIVITY
STARS: LATE-TYPE
STARS: LOW-MASS
STARSPOTS
topic BINARIES: GENERAL
STARS: ACTIVITY
STARS: LATE-TYPE
STARS: LOW-MASS
STARSPOTS
purl_subject.fl_str_mv https://purl.org/becyt/ford/1.7
https://purl.org/becyt/ford/1
dc.description.none.fl_txt_mv Context. There are a variety of different techniques available to estimate the ages of pre-main-sequence stars. Components of physical pairs, thanks to their strict coevality and the mass difference, such as the binary system analyzed in this paper, are best suited to test the effectiveness of these different techniques. Aims. We consider the system WW Psa + TX Psa whose membership of the 25-Myr β Pictoris association has been well established by earlier works. We aim to investigate which age-dating technique provides the best agreement between the age of the system and that of the association. Methods. We have photometrically monitored WW Psa and TX Psa and measured their rotation periods as P = 2.37 d and P = 1.086 d, respectively. We have retrieved their Li equivalent widths from the literature and measured their effective temperatures and luminosities. We investigated whether the ages of these stars derived using three independent techniques, that is based on rotation, Li equivalent widths, and the position in the HR diagram are consistent with the age of the β Pictoris association. Results. We find that the rotation periods and the Li contents of both stars are consistent with the distribution of other bona fide members of the cluster. On the contrary, the isochronal fitting provides similar ages for both stars, but a factor of about four younger than the quoted age of the association, or about 30% younger when the effects of magnetic fields are included. Conclusions. We explore the origin of the discrepant age inferred from isochronal fitting, including the possibilities that either the two components may be unresolved binaries or that the basic stellar parameters of both components are altered by enhanced magnetic activity. The latter is found to be the more reasonable cause, suggesting that age estimates based on Li content are more reliable than isochronal fitting for pre-main-sequence stars with pronounced magnetic activity.
Fil: Messina, S.. Osservatorio Astrofisico Di Catania; Italia
Fil: Santallo, R.. Southern Stars Observatory; Polinesia Francesa
Fil: Tan, T.. Perth Exoplanet Survey Telescope; Australia
Fil: Elliot, P.. European Southern Observatory; Chile
Fil: Feiden, G.. Uppsala Universitet; Suecia
Fil: Buccino, Andrea Paola. Consejo Nacional de Investigaciones Científicas y Técnicas. Oficina de Coordinación Administrativa Ciudad Universitaria. Instituto de Astronomía y Física del Espacio. - Universidad de Buenos Aires. Facultad de Ciencias Exactas y Naturales. Instituto de Astronomía y Física del Espacio; 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. - Universidad de Buenos Aires. Facultad de Ciencias Exactas y Naturales. Instituto de Astronomía y Física del Espacio; Argentina
Fil: Petrucci, Romina Paola. Universidad Nacional de Córdoba. Observatorio Astronómico de Córdoba; Argentina. Consejo Nacional de Investigaciones Científicas y Técnicas. Centro Científico Tecnológico Conicet - Córdoba; Argentina
Fil: Jofré, E.. Universidad Nacional de Córdoba. Observatorio Astronómico de Córdoba; Argentina
description Context. There are a variety of different techniques available to estimate the ages of pre-main-sequence stars. Components of physical pairs, thanks to their strict coevality and the mass difference, such as the binary system analyzed in this paper, are best suited to test the effectiveness of these different techniques. Aims. We consider the system WW Psa + TX Psa whose membership of the 25-Myr β Pictoris association has been well established by earlier works. We aim to investigate which age-dating technique provides the best agreement between the age of the system and that of the association. Methods. We have photometrically monitored WW Psa and TX Psa and measured their rotation periods as P = 2.37 d and P = 1.086 d, respectively. We have retrieved their Li equivalent widths from the literature and measured their effective temperatures and luminosities. We investigated whether the ages of these stars derived using three independent techniques, that is based on rotation, Li equivalent widths, and the position in the HR diagram are consistent with the age of the β Pictoris association. Results. We find that the rotation periods and the Li contents of both stars are consistent with the distribution of other bona fide members of the cluster. On the contrary, the isochronal fitting provides similar ages for both stars, but a factor of about four younger than the quoted age of the association, or about 30% younger when the effects of magnetic fields are included. Conclusions. We explore the origin of the discrepant age inferred from isochronal fitting, including the possibilities that either the two components may be unresolved binaries or that the basic stellar parameters of both components are altered by enhanced magnetic activity. The latter is found to be the more reasonable cause, suggesting that age estimates based on Li content are more reliable than isochronal fitting for pre-main-sequence stars with pronounced magnetic activity.
publishDate 2016
dc.date.none.fl_str_mv 2016-12
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/11336/180085
Messina, S.; Santallo, R.; Tan, T.; Elliot, P.; Feiden, G.; et al.; On the age of the magnetically active WW Psa and TX Psa members of the beta Pictoris association; EDP Sciences; Astronomy and Astrophysics; 601; A54; 12-2016; 1-12
0004-6361
CONICET Digital
CONICET
url http://hdl.handle.net/11336/180085
identifier_str_mv Messina, S.; Santallo, R.; Tan, T.; Elliot, P.; Feiden, G.; et al.; On the age of the magnetically active WW Psa and TX Psa members of the beta Pictoris association; EDP Sciences; Astronomy and Astrophysics; 601; A54; 12-2016; 1-12
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/articles/aa/pdf/2017/05/aa28514-16.pdf
info:eu-repo/semantics/altIdentifier/doi/10.1051/0004-6361/201628514
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 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
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score 12.982451

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