The HD 5980 multiple system: masses and evolutionary status
- Autores
- Koenigsberger, G.; Morrell, Nidia Irene; Hillier, D. J.; Gamen, Roberto Claudio; Schneider, F. R. N.; González Jiménez, N.; Langer, N.; Barbá, Rodolfo Héctor
- Año de publicación
- 2014
- Idioma
- inglés
- Tipo de recurso
- artículo
- Estado
- versión publicada
- Descripción
- New spectroscopic observations of the LBV/WR multiple system HD 5980 in the Small Magellanic Cloud are used to address the question of the masses and evolutionary status of the two very luminous stars in the 19.3 day eclipsing binary system. Two distinct components of the N V 4944 A˚ line are detected in emission and their radial velocity variations are used to derive masses of 61 and 66 M ⊙, under the assumption that binary interaction effects on this atomic transition are negligible. We propose that this binary system is the product of quasi-chemically homogeneous evolution with little or no mass transfer. Thus, both of these binary stars may be candidates for gamma-ray burst progenitors or even pair instability supernovae. Analysis of the photospheric absorption lines belonging to the third-light object in the system confirm that it consists of an O-type star in a 96.56 day eccentric orbit (e = 0.82) around an unseen companion. The 5:1 period ratio and high eccentricities of the two binaries suggest that they may constitute a hierarchical quadruple system.
Instituto de Astrofísica de La Plata
Facultad de Ciencias Astronómicas y Geofísicas - Materia
-
Ciencias Astronómicas
binaries
color figures
eclipsing - stars
evolution - stars
individual (HD 5980) - stars
massive - stars
Wolf-Rayet Online-only material - Nivel de accesibilidad
- acceso abierto
- Condiciones de uso
- http://creativecommons.org/licenses/by-nc-sa/4.0/
- Repositorio
.jpg)
- Institución
- Universidad Nacional de La Plata
- OAI Identificador
- oai:sedici.unlp.edu.ar:10915/85133
Ver los metadatos del registro completo
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The HD 5980 multiple system: masses and evolutionary statusKoenigsberger, G.Morrell, Nidia IreneHillier, D. J.Gamen, Roberto ClaudioSchneider, F. R. N.González Jiménez, N.Langer, N.Barbá, Rodolfo HéctorCiencias Astronómicasbinariescolor figureseclipsing - starsevolution - starsindividual (HD 5980) - starsmassive - starsWolf-Rayet Online-only materialNew spectroscopic observations of the LBV/WR multiple system HD 5980 in the Small Magellanic Cloud are used to address the question of the masses and evolutionary status of the two very luminous stars in the 19.3 day eclipsing binary system. Two distinct components of the N V 4944 A˚ line are detected in emission and their radial velocity variations are used to derive masses of 61 and 66 M ⊙, under the assumption that binary interaction effects on this atomic transition are negligible. We propose that this binary system is the product of quasi-chemically homogeneous evolution with little or no mass transfer. Thus, both of these binary stars may be candidates for gamma-ray burst progenitors or even pair instability supernovae. Analysis of the photospheric absorption lines belonging to the third-light object in the system confirm that it consists of an O-type star in a 96.56 day eccentric orbit (e = 0.82) around an unseen companion. The 5:1 period ratio and high eccentricities of the two binaries suggest that they may constitute a hierarchical quadruple system.Instituto de Astrofísica de La PlataFacultad de Ciencias Astronómicas y Geofísicas2014-09-03info:eu-repo/semantics/articleinfo:eu-repo/semantics/publishedVersionArticulohttp://purl.org/coar/resource_type/c_6501info:ar-repo/semantics/articuloapplication/pdfhttp://sedici.unlp.edu.ar/handle/10915/85133enginfo:eu-repo/semantics/altIdentifier/issn/0004-6256info:eu-repo/semantics/altIdentifier/doi/10.1088/0004-6256/148/4/62info:eu-repo/semantics/openAccesshttp://creativecommons.org/licenses/by-nc-sa/4.0/Creative Commons Attribution-NonCommercial-ShareAlike 4.0 International (CC BY-NC-SA 4.0)reponame:SEDICI (UNLP)instname:Universidad Nacional de La Platainstacron:UNLP2025-10-15T11:08:16Zoai:sedici.unlp.edu.ar:10915/85133Institucionalhttp://sedici.unlp.edu.ar/Universidad públicaNo correspondehttp://sedici.unlp.edu.ar/oai/snrdalira@sedici.unlp.edu.arArgentinaNo correspondeNo correspondeNo correspondeopendoar:13292025-10-15 11:08:16.839SEDICI (UNLP) - Universidad Nacional de La Platafalse |
| dc.title.none.fl_str_mv |
The HD 5980 multiple system: masses and evolutionary status |
| title |
The HD 5980 multiple system: masses and evolutionary status |
| spellingShingle |
The HD 5980 multiple system: masses and evolutionary status Koenigsberger, G. Ciencias Astronómicas binaries color figures eclipsing - stars evolution - stars individual (HD 5980) - stars massive - stars Wolf-Rayet Online-only material |
| title_short |
The HD 5980 multiple system: masses and evolutionary status |
| title_full |
The HD 5980 multiple system: masses and evolutionary status |
| title_fullStr |
The HD 5980 multiple system: masses and evolutionary status |
| title_full_unstemmed |
The HD 5980 multiple system: masses and evolutionary status |
| title_sort |
The HD 5980 multiple system: masses and evolutionary status |
| dc.creator.none.fl_str_mv |
Koenigsberger, G. Morrell, Nidia Irene Hillier, D. J. Gamen, Roberto Claudio Schneider, F. R. N. González Jiménez, N. Langer, N. Barbá, Rodolfo Héctor |
| author |
Koenigsberger, G. |
| author_facet |
Koenigsberger, G. Morrell, Nidia Irene Hillier, D. J. Gamen, Roberto Claudio Schneider, F. R. N. González Jiménez, N. Langer, N. Barbá, Rodolfo Héctor |
| author_role |
author |
| author2 |
Morrell, Nidia Irene Hillier, D. J. Gamen, Roberto Claudio Schneider, F. R. N. González Jiménez, N. Langer, N. Barbá, Rodolfo Héctor |
| author2_role |
author author author author author author author |
| dc.subject.none.fl_str_mv |
Ciencias Astronómicas binaries color figures eclipsing - stars evolution - stars individual (HD 5980) - stars massive - stars Wolf-Rayet Online-only material |
| topic |
Ciencias Astronómicas binaries color figures eclipsing - stars evolution - stars individual (HD 5980) - stars massive - stars Wolf-Rayet Online-only material |
| dc.description.none.fl_txt_mv |
New spectroscopic observations of the LBV/WR multiple system HD 5980 in the Small Magellanic Cloud are used to address the question of the masses and evolutionary status of the two very luminous stars in the 19.3 day eclipsing binary system. Two distinct components of the N V 4944 A˚ line are detected in emission and their radial velocity variations are used to derive masses of 61 and 66 M ⊙, under the assumption that binary interaction effects on this atomic transition are negligible. We propose that this binary system is the product of quasi-chemically homogeneous evolution with little or no mass transfer. Thus, both of these binary stars may be candidates for gamma-ray burst progenitors or even pair instability supernovae. Analysis of the photospheric absorption lines belonging to the third-light object in the system confirm that it consists of an O-type star in a 96.56 day eccentric orbit (e = 0.82) around an unseen companion. The 5:1 period ratio and high eccentricities of the two binaries suggest that they may constitute a hierarchical quadruple system. Instituto de Astrofísica de La Plata Facultad de Ciencias Astronómicas y Geofísicas |
| description |
New spectroscopic observations of the LBV/WR multiple system HD 5980 in the Small Magellanic Cloud are used to address the question of the masses and evolutionary status of the two very luminous stars in the 19.3 day eclipsing binary system. Two distinct components of the N V 4944 A˚ line are detected in emission and their radial velocity variations are used to derive masses of 61 and 66 M ⊙, under the assumption that binary interaction effects on this atomic transition are negligible. We propose that this binary system is the product of quasi-chemically homogeneous evolution with little or no mass transfer. Thus, both of these binary stars may be candidates for gamma-ray burst progenitors or even pair instability supernovae. Analysis of the photospheric absorption lines belonging to the third-light object in the system confirm that it consists of an O-type star in a 96.56 day eccentric orbit (e = 0.82) around an unseen companion. The 5:1 period ratio and high eccentricities of the two binaries suggest that they may constitute a hierarchical quadruple system. |
| publishDate |
2014 |
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2014-09-03 |
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info:eu-repo/semantics/article info:eu-repo/semantics/publishedVersion Articulo http://purl.org/coar/resource_type/c_6501 info:ar-repo/semantics/articulo |
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eng |
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