Identification of a deep contact binary in the field of the globular cluster 47 Tuc

Autores
Liu L.; Qian, S. B.; Fernandez Lajus, Eduardo Eusebio
Año de publicación
2014
Idioma
inglés
Tipo de recurso
artículo
Estado
versión publicada
Descripción
Three light curves of the eclipsing binary V95–47 Tuc were obtained in serval nights from December, 2010 to November, 2011. By analyzing the light curves with the 2010 version of the W-D code, the mass-ratio and the fill-out factor of V95 are determined as 0.164 and 53.8%, respectively. It is sure that this contact binary is a foreground object of the globular cluster 47 Tuc. By comparing to the Dartmouth model isochrones, the masses and the radii of the component stars are estimated, as well as the age and the distance. They are, M1 ¼ 0:97M; M2 ¼ 0:16M; R1 ¼ 1:05R; R2 ¼ 0:49R, Age = 7.0 Gyr and Dist = 1570 pc. The cool spots model is introduced in the BV-band photometric solutions because of the observed O’Connell effect. We compare the two modeling cool spots in size, temperature and position, thinking that they could be the same one. It can be explained as that a cool spot, which is on the surface of the more massive component, shifted 126 degrees along the latitude line from west to east in a year. This phenomenon may be called as starspot migration.
Fil: Liu L.. Chinese Academy Of Sciences; República de China
Fil: Qian, S. B.. Chinese Academy Of Sciences; República de China
Fil: Fernandez Lajus, Eduardo Eusebio. Consejo Nacional de Investigaciones Científicas y Técnicas. Centro Científico Tecnológico la Plata. Instituto de Astrofísica de la Plata; Argentina. Universidad Nacional de la Plata. Facultad de Ciencias Astronómicas y Geofísicas; Argentina
Materia
Eclipsing
V95 47 Tuc
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:11336/10763

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spelling Identification of a deep contact binary in the field of the globular cluster 47 TucLiu L.Qian, S. B.Fernandez Lajus, Eduardo EusebioEclipsingV95 47 Tuchttps://purl.org/becyt/ford/1.3https://purl.org/becyt/ford/1Three light curves of the eclipsing binary V95–47 Tuc were obtained in serval nights from December, 2010 to November, 2011. By analyzing the light curves with the 2010 version of the W-D code, the mass-ratio and the fill-out factor of V95 are determined as 0.164 and 53.8%, respectively. It is sure that this contact binary is a foreground object of the globular cluster 47 Tuc. By comparing to the Dartmouth model isochrones, the masses and the radii of the component stars are estimated, as well as the age and the distance. They are, M1 ¼ 0:97M; M2 ¼ 0:16M; R1 ¼ 1:05R; R2 ¼ 0:49R, Age = 7.0 Gyr and Dist = 1570 pc. The cool spots model is introduced in the BV-band photometric solutions because of the observed O’Connell effect. We compare the two modeling cool spots in size, temperature and position, thinking that they could be the same one. It can be explained as that a cool spot, which is on the surface of the more massive component, shifted 126 degrees along the latitude line from west to east in a year. This phenomenon may be called as starspot migration.Fil: Liu L.. Chinese Academy Of Sciences; República de ChinaFil: Qian, S. B.. Chinese Academy Of Sciences; República de ChinaFil: Fernandez Lajus, Eduardo Eusebio. Consejo Nacional de Investigaciones Científicas y Técnicas. Centro Científico Tecnológico la Plata. Instituto de Astrofísica de la Plata; Argentina. Universidad Nacional de la Plata. Facultad de Ciencias Astronómicas y Geofísicas; ArgentinaElsevier Science2014-01info:eu-repo/semantics/articleinfo:eu-repo/semantics/publishedVersionhttp://purl.org/coar/resource_type/c_6501info:ar-repo/semantics/articuloapplication/pdfapplication/pdfhttp://hdl.handle.net/11336/10763Liu L.; Qian, S. B.; Fernandez Lajus, Eduardo Eusebio; Identification of a deep contact binary in the field of the globular cluster 47 Tuc; Elsevier Science; New Astronomy; 26; 1; 1-2014; 116-1201384-1076enginfo:eu-repo/semantics/altIdentifier/doi/10.1016/j.newast.2013.07.004info:eu-repo/semantics/altIdentifier/url/http://www.sciencedirect.com/science/article/pii/S138410761300081Xinfo:eu-repo/semantics/openAccesshttps://creativecommons.org/licenses/by-nc-sa/2.5/ar/reponame:CONICET Digital (CONICET)instname:Consejo Nacional de Investigaciones Científicas y Técnicas2025-09-29T09:38:03Zoai:ri.conicet.gov.ar:11336/10763instacron: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 09:38:03.352CONICET Digital (CONICET) - Consejo Nacional de Investigaciones Científicas y Técnicasfalse
dc.title.none.fl_str_mv Identification of a deep contact binary in the field of the globular cluster 47 Tuc
title Identification of a deep contact binary in the field of the globular cluster 47 Tuc
spellingShingle Identification of a deep contact binary in the field of the globular cluster 47 Tuc
Liu L.
Eclipsing
V95 47 Tuc
title_short Identification of a deep contact binary in the field of the globular cluster 47 Tuc
title_full Identification of a deep contact binary in the field of the globular cluster 47 Tuc
title_fullStr Identification of a deep contact binary in the field of the globular cluster 47 Tuc
title_full_unstemmed Identification of a deep contact binary in the field of the globular cluster 47 Tuc
title_sort Identification of a deep contact binary in the field of the globular cluster 47 Tuc
dc.creator.none.fl_str_mv Liu L.
Qian, S. B.
Fernandez Lajus, Eduardo Eusebio
author Liu L.
author_facet Liu L.
Qian, S. B.
Fernandez Lajus, Eduardo Eusebio
author_role author
author2 Qian, S. B.
Fernandez Lajus, Eduardo Eusebio
author2_role author
author
dc.subject.none.fl_str_mv Eclipsing
V95 47 Tuc
topic Eclipsing
V95 47 Tuc
purl_subject.fl_str_mv https://purl.org/becyt/ford/1.3
https://purl.org/becyt/ford/1
dc.description.none.fl_txt_mv Three light curves of the eclipsing binary V95–47 Tuc were obtained in serval nights from December, 2010 to November, 2011. By analyzing the light curves with the 2010 version of the W-D code, the mass-ratio and the fill-out factor of V95 are determined as 0.164 and 53.8%, respectively. It is sure that this contact binary is a foreground object of the globular cluster 47 Tuc. By comparing to the Dartmouth model isochrones, the masses and the radii of the component stars are estimated, as well as the age and the distance. They are, M1 ¼ 0:97M; M2 ¼ 0:16M; R1 ¼ 1:05R; R2 ¼ 0:49R, Age = 7.0 Gyr and Dist = 1570 pc. The cool spots model is introduced in the BV-band photometric solutions because of the observed O’Connell effect. We compare the two modeling cool spots in size, temperature and position, thinking that they could be the same one. It can be explained as that a cool spot, which is on the surface of the more massive component, shifted 126 degrees along the latitude line from west to east in a year. This phenomenon may be called as starspot migration.
Fil: Liu L.. Chinese Academy Of Sciences; República de China
Fil: Qian, S. B.. Chinese Academy Of Sciences; República de China
Fil: Fernandez Lajus, Eduardo Eusebio. Consejo Nacional de Investigaciones Científicas y Técnicas. Centro Científico Tecnológico la Plata. Instituto de Astrofísica de la Plata; Argentina. Universidad Nacional de la Plata. Facultad de Ciencias Astronómicas y Geofísicas; Argentina
description Three light curves of the eclipsing binary V95–47 Tuc were obtained in serval nights from December, 2010 to November, 2011. By analyzing the light curves with the 2010 version of the W-D code, the mass-ratio and the fill-out factor of V95 are determined as 0.164 and 53.8%, respectively. It is sure that this contact binary is a foreground object of the globular cluster 47 Tuc. By comparing to the Dartmouth model isochrones, the masses and the radii of the component stars are estimated, as well as the age and the distance. They are, M1 ¼ 0:97M; M2 ¼ 0:16M; R1 ¼ 1:05R; R2 ¼ 0:49R, Age = 7.0 Gyr and Dist = 1570 pc. The cool spots model is introduced in the BV-band photometric solutions because of the observed O’Connell effect. We compare the two modeling cool spots in size, temperature and position, thinking that they could be the same one. It can be explained as that a cool spot, which is on the surface of the more massive component, shifted 126 degrees along the latitude line from west to east in a year. This phenomenon may be called as starspot migration.
publishDate 2014
dc.date.none.fl_str_mv 2014-01
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/11336/10763
Liu L.; Qian, S. B.; Fernandez Lajus, Eduardo Eusebio; Identification of a deep contact binary in the field of the globular cluster 47 Tuc; Elsevier Science; New Astronomy; 26; 1; 1-2014; 116-120
1384-1076
url http://hdl.handle.net/11336/10763
identifier_str_mv Liu L.; Qian, S. B.; Fernandez Lajus, Eduardo Eusebio; Identification of a deep contact binary in the field of the globular cluster 47 Tuc; Elsevier Science; New Astronomy; 26; 1; 1-2014; 116-120
1384-1076
dc.language.none.fl_str_mv eng
language eng
dc.relation.none.fl_str_mv info:eu-repo/semantics/altIdentifier/doi/10.1016/j.newast.2013.07.004
info:eu-repo/semantics/altIdentifier/url/http://www.sciencedirect.com/science/article/pii/S138410761300081X
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 Elsevier Science
publisher.none.fl_str_mv Elsevier Science
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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