The new Wolf-Rayet binary system WR62a

Autores
Collado, Ana Elisa; Gamen, Roberto Claudio; Barba, Rodolfo Hector
Año de publicación
2013
Idioma
inglés
Tipo de recurso
artículo
Estado
versión publicada
Descripción
A significant number of the Wolf-Rayet stars seem to be binary or multiple systems, but the nature of many of them is still unknown. Dedicated monitoring of WR stars favours the discovery of new systems. Aims. We explore the possibility that WR62a is a binary system. Methods. We analysed the spectra of WR62a, obtained between 2002 and 2010, to look for radial-velocity and spectral variations that would suggest there is a binary component. We searched for periodicities in the measured radial velocities and determined orbital solutions. A period search was also performed on the “All-Sky Automated Survey” photometry. Results. We find that WR62a is a double-lined spectroscopic binary with a WN5 primary star and an O 5.5–6 type secondary component in orbit with a period of 9.1447 d. The minimum masses range between 21 and 23 M for the WN star and between 39 and 42 M for the O-type star, thus indicating that the WN star is less massive than the O-type component. We detect a phase shift in the radial-velocity curve of the He ii λ4686 emission line relative to the other emission line curves. The equivalent width of this emission line shows a minimum value when the WN star passes in front of the system. The analysis of the ASAS photometry confirms the spectroscopic periodicity, presenting a minimum at the same phase.
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
Fil: Gamen, Roberto Claudio. Consejo Nacional de Investigaciones Científicas y Técnicas. Centro Científico Tecnológico Conicet - La Plata. Instituto de Astrofísica La Plata. Universidad Nacional de La Plata. Facultad de Ciencias Astronómicas y Geofísicas. Instituto de Astrofísica la Plata; Argentina
Fil: Barba, Rodolfo Hector. 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. Universidad de la Serena; Chile
Materia
binaries: spectroscopic
stars: individual: SMSNPL11 (=WR62a)
stars: Wolf-Rayet
stars: fundamental parameters
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:11336/21493
Acceder
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network_acronym_str CONICETDig
repository_id_str 3498
network_name_str CONICET Digital (CONICET)
spelling The new Wolf-Rayet binary system WR62aCollado, Ana ElisaGamen, Roberto ClaudioBarba, Rodolfo Hectorbinaries: spectroscopicstars: individual: SMSNPL11 (=WR62a)stars: Wolf-Rayetstars: fundamental parametershttps://purl.org/becyt/ford/1.3https://purl.org/becyt/ford/1A significant number of the Wolf-Rayet stars seem to be binary or multiple systems, but the nature of many of them is still unknown. Dedicated monitoring of WR stars favours the discovery of new systems. Aims. We explore the possibility that WR62a is a binary system. Methods. We analysed the spectra of WR62a, obtained between 2002 and 2010, to look for radial-velocity and spectral variations that would suggest there is a binary component. We searched for periodicities in the measured radial velocities and determined orbital solutions. A period search was also performed on the “All-Sky Automated Survey” photometry. Results. We find that WR62a is a double-lined spectroscopic binary with a WN5 primary star and an O 5.5–6 type secondary component in orbit with a period of 9.1447 d. The minimum masses range between 21 and 23 M for the WN star and between 39 and 42 M for the O-type star, thus indicating that the WN star is less massive than the O-type component. We detect a phase shift in the radial-velocity curve of the He ii λ4686 emission line relative to the other emission line curves. The equivalent width of this emission line shows a minimum value when the WN star passes in front of the system. The analysis of the ASAS photometry confirms the spectroscopic periodicity, presenting a minimum at the same phase.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; ArgentinaFil: Gamen, Roberto Claudio. Consejo Nacional de Investigaciones Científicas y Técnicas. Centro Científico Tecnológico Conicet - La Plata. Instituto de Astrofísica La Plata. Universidad Nacional de La Plata. Facultad de Ciencias Astronómicas y Geofísicas. Instituto de Astrofísica la Plata; ArgentinaFil: Barba, Rodolfo Hector. 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. Universidad de la Serena; ChileEdp Sciences2013-04info:eu-repo/semantics/articleinfo:eu-repo/semantics/publishedVersionhttp://purl.org/coar/resource_type/c_6501info:ar-repo/semantics/articuloapplication/pdfapplication/pdfhttp://hdl.handle.net/11336/21493Collado, Ana Elisa; Gamen, Roberto Claudio; Barba, Rodolfo Hector; The new Wolf-Rayet binary system WR62a; Edp Sciences; Astronomy And Astrophysics; 552; 4-2013; 1-7; 220004-6361CONICET DigitalCONICETenginfo:eu-repo/semantics/altIdentifier/doi/10.1051/0004-6361/201118460info:eu-repo/semantics/altIdentifier/url/https://www.aanda.org/articles/aa/abs/2013/04/aa18460-11/aa18460-11.htmlinfo:eu-repo/semantics/openAccesshttps://creativecommons.org/licenses/by-nc-sa/2.5/ar/reponame:CONICET Digital (CONICET)instname:Consejo Nacional de Investigaciones Científicas y Técnicas2025-09-03T09:53:48Zoai:ri.conicet.gov.ar:11336/21493instacron: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:34982025-09-03 09:53:49.143CONICET Digital (CONICET) - Consejo Nacional de Investigaciones Científicas y Técnicasfalse
dc.title.none.fl_str_mv The new Wolf-Rayet binary system WR62a
title The new Wolf-Rayet binary system WR62a
spellingShingle The new Wolf-Rayet binary system WR62a
Collado, Ana Elisa
binaries: spectroscopic
stars: individual: SMSNPL11 (=WR62a)
stars: Wolf-Rayet
stars: fundamental parameters
title_short The new Wolf-Rayet binary system WR62a
title_full The new Wolf-Rayet binary system WR62a
title_fullStr The new Wolf-Rayet binary system WR62a
title_full_unstemmed The new Wolf-Rayet binary system WR62a
title_sort The new Wolf-Rayet binary system WR62a
dc.creator.none.fl_str_mv Collado, Ana Elisa
Gamen, Roberto Claudio
Barba, Rodolfo Hector
author Collado, Ana Elisa
author_facet Collado, Ana Elisa
Gamen, Roberto Claudio
Barba, Rodolfo Hector
author_role author
author2 Gamen, Roberto Claudio
Barba, Rodolfo Hector
author2_role author
author
dc.subject.none.fl_str_mv binaries: spectroscopic
stars: individual: SMSNPL11 (=WR62a)
stars: Wolf-Rayet
stars: fundamental parameters
topic binaries: spectroscopic
stars: individual: SMSNPL11 (=WR62a)
stars: Wolf-Rayet
stars: fundamental parameters
purl_subject.fl_str_mv https://purl.org/becyt/ford/1.3
https://purl.org/becyt/ford/1
dc.description.none.fl_txt_mv A significant number of the Wolf-Rayet stars seem to be binary or multiple systems, but the nature of many of them is still unknown. Dedicated monitoring of WR stars favours the discovery of new systems. Aims. We explore the possibility that WR62a is a binary system. Methods. We analysed the spectra of WR62a, obtained between 2002 and 2010, to look for radial-velocity and spectral variations that would suggest there is a binary component. We searched for periodicities in the measured radial velocities and determined orbital solutions. A period search was also performed on the “All-Sky Automated Survey” photometry. Results. We find that WR62a is a double-lined spectroscopic binary with a WN5 primary star and an O 5.5–6 type secondary component in orbit with a period of 9.1447 d. The minimum masses range between 21 and 23 M for the WN star and between 39 and 42 M for the O-type star, thus indicating that the WN star is less massive than the O-type component. We detect a phase shift in the radial-velocity curve of the He ii λ4686 emission line relative to the other emission line curves. The equivalent width of this emission line shows a minimum value when the WN star passes in front of the system. The analysis of the ASAS photometry confirms the spectroscopic periodicity, presenting a minimum at the same phase.
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
Fil: Gamen, Roberto Claudio. Consejo Nacional de Investigaciones Científicas y Técnicas. Centro Científico Tecnológico Conicet - La Plata. Instituto de Astrofísica La Plata. Universidad Nacional de La Plata. Facultad de Ciencias Astronómicas y Geofísicas. Instituto de Astrofísica la Plata; Argentina
Fil: Barba, Rodolfo Hector. 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. Universidad de la Serena; Chile
description A significant number of the Wolf-Rayet stars seem to be binary or multiple systems, but the nature of many of them is still unknown. Dedicated monitoring of WR stars favours the discovery of new systems. Aims. We explore the possibility that WR62a is a binary system. Methods. We analysed the spectra of WR62a, obtained between 2002 and 2010, to look for radial-velocity and spectral variations that would suggest there is a binary component. We searched for periodicities in the measured radial velocities and determined orbital solutions. A period search was also performed on the “All-Sky Automated Survey” photometry. Results. We find that WR62a is a double-lined spectroscopic binary with a WN5 primary star and an O 5.5–6 type secondary component in orbit with a period of 9.1447 d. The minimum masses range between 21 and 23 M for the WN star and between 39 and 42 M for the O-type star, thus indicating that the WN star is less massive than the O-type component. We detect a phase shift in the radial-velocity curve of the He ii λ4686 emission line relative to the other emission line curves. The equivalent width of this emission line shows a minimum value when the WN star passes in front of the system. The analysis of the ASAS photometry confirms the spectroscopic periodicity, presenting a minimum at the same phase.
publishDate 2013
dc.date.none.fl_str_mv 2013-04
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/11336/21493
Collado, Ana Elisa; Gamen, Roberto Claudio; Barba, Rodolfo Hector; The new Wolf-Rayet binary system WR62a; Edp Sciences; Astronomy And Astrophysics; 552; 4-2013; 1-7; 22
0004-6361
CONICET Digital
CONICET
url http://hdl.handle.net/11336/21493
identifier_str_mv Collado, Ana Elisa; Gamen, Roberto Claudio; Barba, Rodolfo Hector; The new Wolf-Rayet binary system WR62a; Edp Sciences; Astronomy And Astrophysics; 552; 4-2013; 1-7; 22
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/doi/10.1051/0004-6361/201118460
info:eu-repo/semantics/altIdentifier/url/https://www.aanda.org/articles/aa/abs/2013/04/aa18460-11/aa18460-11.html
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 13.13397

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