The enigmatic binary system HD 5980

Autores
Hillier, Desmond John; Koenigsberger, Gloria; Nazé, Yaël; Morrell, Nidia Irene; Barbá, Rodolfo; Gamen, Roberto Claudio
Año de publicación
2019
Idioma
inglés
Tipo de recurso
artículo
Estado
versión publicada
Descripción
The Small Magellanic Cloud multiple system HD 5980 contains a luminous blue variable (LBV) that underwent a major eruption in 1994, and whose current spectrum is that of a hydrogen-rich Wolf-Rayet (WR) star. Since the eruption, the wind mass-loss rate has been declining while wind speeds have been steadily increasing. Observations obtained in 2014 when Star A (the LBV) eclipses Star B indicate that the fitted mass-loss rate and luminosity have reached the lowest values ever determined for such spectra: dot{M} = 4.5 × 10-5M_☉ yr^{-1}, L = 1.7 × 106 L☉. In addition, the radius of the LBV´s continuum-emitting region is similar to that derived from the eclipse light curves of the late 1970s. Hence, it appears to have attained a similar `low´ state to that of the late 1970s. While a good fit to the emission spectrum is obtained using a CMFGEN model, there are discrepancies in the UV. In particular, the extent of the observed absorption profiles is ̃1000 km s-1 greater than predicted by the emission-line intensities. Further, HST UV observations obtained in 2016, when Star A is eclipsed by Star B, show unusual P Cygni profiles that are not easily explained. Surprisingly the 2016 emission-line spectrum is similar to that at the opposite eclipse obtained in 2014. The complex UV profiles are likely to arise as a consequence of the dynamics of the wind-wind collision and radiative braking, both of which will cause significant departures from spherical symmetry, and have a strong orbital phase dependence. However, other scenarios, such as intrinsically aspherical winds, cannot be ruled out.
Fil: Hillier, Desmond John. University of Pittsburgh; Estados Unidos
Fil: Koenigsberger, Gloria. Universidad Nacional Autónoma de México; México
Fil: Nazé, Yaël. Université de Liège; Bélgica
Fil: Morrell, Nidia Irene. Carnegie Institution. Observatorio Las Campanas; Chile. 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: Barbá, Rodolfo. Universidad de La Serena; Chile
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
Materia
binaries: eclipsing
stars: individual(HD 5980)
stars: Wolf-Rayet
stars: winds
outflows
stars: mass-loss
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:11336/125384
Acceder
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oai_identifier_str oai:ri.conicet.gov.ar:11336/125384
network_acronym_str CONICETDig
repository_id_str 3498
network_name_str CONICET Digital (CONICET)
spelling The enigmatic binary system HD 5980Hillier, Desmond JohnKoenigsberger, GloriaNazé, YaëlMorrell, Nidia IreneBarbá, RodolfoGamen, Roberto Claudiobinaries: eclipsingstars: individual(HD 5980)stars: Wolf-Rayetstars: windsoutflowsstars: mass-losshttps://purl.org/becyt/ford/1.3https://purl.org/becyt/ford/1The Small Magellanic Cloud multiple system HD 5980 contains a luminous blue variable (LBV) that underwent a major eruption in 1994, and whose current spectrum is that of a hydrogen-rich Wolf-Rayet (WR) star. Since the eruption, the wind mass-loss rate has been declining while wind speeds have been steadily increasing. Observations obtained in 2014 when Star A (the LBV) eclipses Star B indicate that the fitted mass-loss rate and luminosity have reached the lowest values ever determined for such spectra: dot{M} = 4.5 × 10-5M_☉ yr^{-1}, L = 1.7 × 106 L☉. In addition, the radius of the LBV´s continuum-emitting region is similar to that derived from the eclipse light curves of the late 1970s. Hence, it appears to have attained a similar `low´ state to that of the late 1970s. While a good fit to the emission spectrum is obtained using a CMFGEN model, there are discrepancies in the UV. In particular, the extent of the observed absorption profiles is ̃1000 km s-1 greater than predicted by the emission-line intensities. Further, HST UV observations obtained in 2016, when Star A is eclipsed by Star B, show unusual P Cygni profiles that are not easily explained. Surprisingly the 2016 emission-line spectrum is similar to that at the opposite eclipse obtained in 2014. The complex UV profiles are likely to arise as a consequence of the dynamics of the wind-wind collision and radiative braking, both of which will cause significant departures from spherical symmetry, and have a strong orbital phase dependence. However, other scenarios, such as intrinsically aspherical winds, cannot be ruled out.Fil: Hillier, Desmond John. University of Pittsburgh; Estados UnidosFil: Koenigsberger, Gloria. Universidad Nacional Autónoma de México; MéxicoFil: Nazé, Yaël. Université de Liège; BélgicaFil: Morrell, Nidia Irene. Carnegie Institution. Observatorio Las Campanas; Chile. 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: Barbá, Rodolfo. Universidad de La Serena; ChileFil: 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; ArgentinaWiley Blackwell Publishing, Inc2019-03-19info:eu-repo/semantics/articleinfo:eu-repo/semantics/publishedVersionhttp://purl.org/coar/resource_type/c_6501info:ar-repo/semantics/articuloapplication/pdfapplication/pdfhttp://hdl.handle.net/11336/125384Hillier, Desmond John; Koenigsberger, Gloria; Nazé, Yaël; Morrell, Nidia Irene; Barbá, Rodolfo; et al.; The enigmatic binary system HD 5980; Wiley Blackwell Publishing, Inc; Monthly Notices of the Royal Astronomical Society; 486; 1; 19-3-2019; 725-7420035-8711CONICET DigitalCONICETenginfo:eu-repo/semantics/altIdentifier/url/https://academic.oup.com/mnras/article/486/1/725/5393415info:eu-repo/semantics/altIdentifier/doi/10.1093/mnras/stz808info:eu-repo/semantics/openAccesshttps://creativecommons.org/licenses/by-nc-sa/2.5/ar/reponame:CONICET Digital (CONICET)instname:Consejo Nacional de Investigaciones Científicas y Técnicas2025-09-29T10:43:44Zoai:ri.conicet.gov.ar:11336/125384instacron: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 10:43:45.234CONICET Digital (CONICET) - Consejo Nacional de Investigaciones Científicas y Técnicasfalse
dc.title.none.fl_str_mv The enigmatic binary system HD 5980
title The enigmatic binary system HD 5980
spellingShingle The enigmatic binary system HD 5980
Hillier, Desmond John
binaries: eclipsing
stars: individual(HD 5980)
stars: Wolf-Rayet
stars: winds
outflows
stars: mass-loss
title_short The enigmatic binary system HD 5980
title_full The enigmatic binary system HD 5980
title_fullStr The enigmatic binary system HD 5980
title_full_unstemmed The enigmatic binary system HD 5980
title_sort The enigmatic binary system HD 5980
dc.creator.none.fl_str_mv Hillier, Desmond John
Koenigsberger, Gloria
Nazé, Yaël
Morrell, Nidia Irene
Barbá, Rodolfo
Gamen, Roberto Claudio
author Hillier, Desmond John
author_facet Hillier, Desmond John
Koenigsberger, Gloria
Nazé, Yaël
Morrell, Nidia Irene
Barbá, Rodolfo
Gamen, Roberto Claudio
author_role author
author2 Koenigsberger, Gloria
Nazé, Yaël
Morrell, Nidia Irene
Barbá, Rodolfo
Gamen, Roberto Claudio
author2_role author
author
author
author
author
dc.subject.none.fl_str_mv binaries: eclipsing
stars: individual(HD 5980)
stars: Wolf-Rayet
stars: winds
outflows
stars: mass-loss
topic binaries: eclipsing
stars: individual(HD 5980)
stars: Wolf-Rayet
stars: winds
outflows
stars: mass-loss
purl_subject.fl_str_mv https://purl.org/becyt/ford/1.3
https://purl.org/becyt/ford/1
dc.description.none.fl_txt_mv The Small Magellanic Cloud multiple system HD 5980 contains a luminous blue variable (LBV) that underwent a major eruption in 1994, and whose current spectrum is that of a hydrogen-rich Wolf-Rayet (WR) star. Since the eruption, the wind mass-loss rate has been declining while wind speeds have been steadily increasing. Observations obtained in 2014 when Star A (the LBV) eclipses Star B indicate that the fitted mass-loss rate and luminosity have reached the lowest values ever determined for such spectra: dot{M} = 4.5 × 10-5M_☉ yr^{-1}, L = 1.7 × 106 L☉. In addition, the radius of the LBV´s continuum-emitting region is similar to that derived from the eclipse light curves of the late 1970s. Hence, it appears to have attained a similar `low´ state to that of the late 1970s. While a good fit to the emission spectrum is obtained using a CMFGEN model, there are discrepancies in the UV. In particular, the extent of the observed absorption profiles is ̃1000 km s-1 greater than predicted by the emission-line intensities. Further, HST UV observations obtained in 2016, when Star A is eclipsed by Star B, show unusual P Cygni profiles that are not easily explained. Surprisingly the 2016 emission-line spectrum is similar to that at the opposite eclipse obtained in 2014. The complex UV profiles are likely to arise as a consequence of the dynamics of the wind-wind collision and radiative braking, both of which will cause significant departures from spherical symmetry, and have a strong orbital phase dependence. However, other scenarios, such as intrinsically aspherical winds, cannot be ruled out.
Fil: Hillier, Desmond John. University of Pittsburgh; Estados Unidos
Fil: Koenigsberger, Gloria. Universidad Nacional Autónoma de México; México
Fil: Nazé, Yaël. Université de Liège; Bélgica
Fil: Morrell, Nidia Irene. Carnegie Institution. Observatorio Las Campanas; Chile. 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: Barbá, Rodolfo. Universidad de La Serena; Chile
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
description The Small Magellanic Cloud multiple system HD 5980 contains a luminous blue variable (LBV) that underwent a major eruption in 1994, and whose current spectrum is that of a hydrogen-rich Wolf-Rayet (WR) star. Since the eruption, the wind mass-loss rate has been declining while wind speeds have been steadily increasing. Observations obtained in 2014 when Star A (the LBV) eclipses Star B indicate that the fitted mass-loss rate and luminosity have reached the lowest values ever determined for such spectra: dot{M} = 4.5 × 10-5M_☉ yr^{-1}, L = 1.7 × 106 L☉. In addition, the radius of the LBV´s continuum-emitting region is similar to that derived from the eclipse light curves of the late 1970s. Hence, it appears to have attained a similar `low´ state to that of the late 1970s. While a good fit to the emission spectrum is obtained using a CMFGEN model, there are discrepancies in the UV. In particular, the extent of the observed absorption profiles is ̃1000 km s-1 greater than predicted by the emission-line intensities. Further, HST UV observations obtained in 2016, when Star A is eclipsed by Star B, show unusual P Cygni profiles that are not easily explained. Surprisingly the 2016 emission-line spectrum is similar to that at the opposite eclipse obtained in 2014. The complex UV profiles are likely to arise as a consequence of the dynamics of the wind-wind collision and radiative braking, both of which will cause significant departures from spherical symmetry, and have a strong orbital phase dependence. However, other scenarios, such as intrinsically aspherical winds, cannot be ruled out.
publishDate 2019
dc.date.none.fl_str_mv 2019-03-19
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/11336/125384
Hillier, Desmond John; Koenigsberger, Gloria; Nazé, Yaël; Morrell, Nidia Irene; Barbá, Rodolfo; et al.; The enigmatic binary system HD 5980; Wiley Blackwell Publishing, Inc; Monthly Notices of the Royal Astronomical Society; 486; 1; 19-3-2019; 725-742
0035-8711
CONICET Digital
CONICET
url http://hdl.handle.net/11336/125384
identifier_str_mv Hillier, Desmond John; Koenigsberger, Gloria; Nazé, Yaël; Morrell, Nidia Irene; Barbá, Rodolfo; et al.; The enigmatic binary system HD 5980; Wiley Blackwell Publishing, Inc; Monthly Notices of the Royal Astronomical Society; 486; 1; 19-3-2019; 725-742
0035-8711
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://academic.oup.com/mnras/article/486/1/725/5393415
info:eu-repo/semantics/altIdentifier/doi/10.1093/mnras/stz808
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 Wiley Blackwell Publishing, Inc
publisher.none.fl_str_mv Wiley Blackwell Publishing, Inc
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 13.070432

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