Fundamental parameters of the massive eclipsing binary HM1 8
- Autores
- Rodríguez, Cinthya Nazarena; Ferrero Sosa, Gabriel Antonio; Benvenuto, Omar Gustavo; Gamen, Roberto Claudio; Morrell, Nidia Irene; Barbá, Rodolfo Héctor; Arias, Julia Inés; Massey, P.
- Año de publicación
- 2021
- Idioma
- inglés
- Tipo de recurso
- artículo
- Estado
- versión publicada
- Descripción
- We present a comprehensive study of the massive binary system HM1 8, based on multi-epoch high-resolution spectroscopy, V-band photometry, and archival X-ray data. Spectra from the OWN Survey, a high-resolution optical monitoring of Southern O and WN stars, are used to analyse the spectral morphology and perform quantitative spectroscopic analysis of both stellar components. The primary and secondary components are classified as O4.5 IV(f) and O9.7 V, respectively. From a radial velocity (RV) study, we derived a set of orbital parameters for the system. We found an eccentric orbit (e = 0.14 ± 0.01) with a period of P = 5.87820 ± 0.00008 d. Through the simultaneous analysis of the RVs and the V-band light curve, we derived an orbital +0.5 inclination of 70.0◦ ± 2.0 and stellar masses of Ma = 33.6+1.4 −1.2 M¯ for the primary, and Mb = 17.7−0.7 M¯ for the secondary. The components show projected rotational velocities v a sin i = 105 ± 14 km s and v b sin i = 82 ± 15 km s−1 , respectively. A tidal evolution analysis is also performed and found to be in agreement with the orbital characteristics. Finally, the available X-ray observations show no evidence of a colliding winds region; therefore, the X-ray emission is attributed to stellar winds.
Facultad de Ciencias Astronómicas y Geofísicas
Instituto de Astrofísica de La Plata - Materia
-
Ciencias Astronómicas
binaries: close
binaries: eclipsing
stars: early-type
stars: fundamental parameters
stars: individual: HM1 8 - Nivel de accesibilidad
- acceso abierto
- Condiciones de uso
- http://creativecommons.org/licenses/by-nc-nd/4.0/
- Repositorio
.jpg)
- Institución
- Universidad Nacional de La Plata
- OAI Identificador
- oai:sedici.unlp.edu.ar:10915/191720
Ver los metadatos del registro completo
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Fundamental parameters of the massive eclipsing binary HM1 8Rodríguez, Cinthya NazarenaFerrero Sosa, Gabriel AntonioBenvenuto, Omar GustavoGamen, Roberto ClaudioMorrell, Nidia IreneBarbá, Rodolfo HéctorArias, Julia InésMassey, P.Ciencias Astronómicasbinaries: closebinaries: eclipsingstars: early-typestars: fundamental parametersstars: individual: HM1 8We present a comprehensive study of the massive binary system HM1 8, based on multi-epoch high-resolution spectroscopy, V-band photometry, and archival X-ray data. Spectra from the OWN Survey, a high-resolution optical monitoring of Southern O and WN stars, are used to analyse the spectral morphology and perform quantitative spectroscopic analysis of both stellar components. The primary and secondary components are classified as O4.5 IV(f) and O9.7 V, respectively. From a radial velocity (RV) study, we derived a set of orbital parameters for the system. We found an eccentric orbit (e = 0.14 ± 0.01) with a period of P = 5.87820 ± 0.00008 d. Through the simultaneous analysis of the RVs and the V-band light curve, we derived an orbital +0.5 inclination of 70.0◦ ± 2.0 and stellar masses of Ma = 33.6+1.4 −1.2 M¯ for the primary, and Mb = 17.7−0.7 M¯ for the secondary. The components show projected rotational velocities v a sin i = 105 ± 14 km s and v b sin i = 82 ± 15 km s−1 , respectively. A tidal evolution analysis is also performed and found to be in agreement with the orbital characteristics. Finally, the available X-ray observations show no evidence of a colliding winds region; therefore, the X-ray emission is attributed to stellar winds.Facultad de Ciencias Astronómicas y GeofísicasInstituto de Astrofísica de La Plata2021-12info:eu-repo/semantics/articleinfo:eu-repo/semantics/publishedVersionArticulohttp://purl.org/coar/resource_type/c_6501info:ar-repo/semantics/articuloapplication/pdf2179–2193http://sedici.unlp.edu.ar/handle/10915/191720enginfo:eu-repo/semantics/altIdentifier/issn/1365-2966info:eu-repo/semantics/altIdentifier/doi/10.1093/mnras/stab2699info:eu-repo/semantics/openAccesshttp://creativecommons.org/licenses/by-nc-nd/4.0/Creative Commons Attribution-NonCommercial-NoDerivatives 4.0 International (CC BY-NC-ND 4.0)reponame:SEDICI (UNLP)instname:Universidad Nacional de La Platainstacron:UNLP2026-05-13T12:59:18Zoai:sedici.unlp.edu.ar:10915/191720Institucionalhttp://sedici.unlp.edu.ar/Universidad públicaNo correspondehttp://sedici.unlp.edu.ar/oai/snrdalira@sedici.unlp.edu.arArgentinaNo correspondeNo correspondeNo correspondeopendoar:13292026-05-13 12:59:18.588SEDICI (UNLP) - Universidad Nacional de La Platafalse |
| dc.title.none.fl_str_mv |
Fundamental parameters of the massive eclipsing binary HM1 8 |
| title |
Fundamental parameters of the massive eclipsing binary HM1 8 |
| spellingShingle |
Fundamental parameters of the massive eclipsing binary HM1 8 Rodríguez, Cinthya Nazarena Ciencias Astronómicas binaries: close binaries: eclipsing stars: early-type stars: fundamental parameters stars: individual: HM1 8 |
| title_short |
Fundamental parameters of the massive eclipsing binary HM1 8 |
| title_full |
Fundamental parameters of the massive eclipsing binary HM1 8 |
| title_fullStr |
Fundamental parameters of the massive eclipsing binary HM1 8 |
| title_full_unstemmed |
Fundamental parameters of the massive eclipsing binary HM1 8 |
| title_sort |
Fundamental parameters of the massive eclipsing binary HM1 8 |
| dc.creator.none.fl_str_mv |
Rodríguez, Cinthya Nazarena Ferrero Sosa, Gabriel Antonio Benvenuto, Omar Gustavo Gamen, Roberto Claudio Morrell, Nidia Irene Barbá, Rodolfo Héctor Arias, Julia Inés Massey, P. |
| author |
Rodríguez, Cinthya Nazarena |
| author_facet |
Rodríguez, Cinthya Nazarena Ferrero Sosa, Gabriel Antonio Benvenuto, Omar Gustavo Gamen, Roberto Claudio Morrell, Nidia Irene Barbá, Rodolfo Héctor Arias, Julia Inés Massey, P. |
| author_role |
author |
| author2 |
Ferrero Sosa, Gabriel Antonio Benvenuto, Omar Gustavo Gamen, Roberto Claudio Morrell, Nidia Irene Barbá, Rodolfo Héctor Arias, Julia Inés Massey, P. |
| author2_role |
author author author author author author author |
| dc.subject.none.fl_str_mv |
Ciencias Astronómicas binaries: close binaries: eclipsing stars: early-type stars: fundamental parameters stars: individual: HM1 8 |
| topic |
Ciencias Astronómicas binaries: close binaries: eclipsing stars: early-type stars: fundamental parameters stars: individual: HM1 8 |
| dc.description.none.fl_txt_mv |
We present a comprehensive study of the massive binary system HM1 8, based on multi-epoch high-resolution spectroscopy, V-band photometry, and archival X-ray data. Spectra from the OWN Survey, a high-resolution optical monitoring of Southern O and WN stars, are used to analyse the spectral morphology and perform quantitative spectroscopic analysis of both stellar components. The primary and secondary components are classified as O4.5 IV(f) and O9.7 V, respectively. From a radial velocity (RV) study, we derived a set of orbital parameters for the system. We found an eccentric orbit (e = 0.14 ± 0.01) with a period of P = 5.87820 ± 0.00008 d. Through the simultaneous analysis of the RVs and the V-band light curve, we derived an orbital +0.5 inclination of 70.0◦ ± 2.0 and stellar masses of Ma = 33.6+1.4 −1.2 M¯ for the primary, and Mb = 17.7−0.7 M¯ for the secondary. The components show projected rotational velocities v a sin i = 105 ± 14 km s and v b sin i = 82 ± 15 km s−1 , respectively. A tidal evolution analysis is also performed and found to be in agreement with the orbital characteristics. Finally, the available X-ray observations show no evidence of a colliding winds region; therefore, the X-ray emission is attributed to stellar winds. Facultad de Ciencias Astronómicas y Geofísicas Instituto de Astrofísica de La Plata |
| description |
We present a comprehensive study of the massive binary system HM1 8, based on multi-epoch high-resolution spectroscopy, V-band photometry, and archival X-ray data. Spectra from the OWN Survey, a high-resolution optical monitoring of Southern O and WN stars, are used to analyse the spectral morphology and perform quantitative spectroscopic analysis of both stellar components. The primary and secondary components are classified as O4.5 IV(f) and O9.7 V, respectively. From a radial velocity (RV) study, we derived a set of orbital parameters for the system. We found an eccentric orbit (e = 0.14 ± 0.01) with a period of P = 5.87820 ± 0.00008 d. Through the simultaneous analysis of the RVs and the V-band light curve, we derived an orbital +0.5 inclination of 70.0◦ ± 2.0 and stellar masses of Ma = 33.6+1.4 −1.2 M¯ for the primary, and Mb = 17.7−0.7 M¯ for the secondary. The components show projected rotational velocities v a sin i = 105 ± 14 km s and v b sin i = 82 ± 15 km s−1 , respectively. A tidal evolution analysis is also performed and found to be in agreement with the orbital characteristics. Finally, the available X-ray observations show no evidence of a colliding winds region; therefore, the X-ray emission is attributed to stellar winds. |
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2021 |
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2021-12 |
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