Chemical fingerprints of He-sdO stars
- Autores
- Schindewolf, Markus; Németh, Peter; Heber, Ulrich; Battich, Tiara; Miller Bertolami, Marcelo Miguel; Latour, Marilyn
- Año de publicación
- 2018
- Idioma
- inglés
- Tipo de recurso
- artículo
- Estado
- versión publicada
- Descripción
- The chemical composition of helium-rich hot subluminous O stars plays an important role to understand and model their formation history. We present a spectroscopic analysis of four He-sdO stars,CD-31∘ 4800, [CW83] 0904- 02, LSS 1274 and LS IV +10∘ 9. The analysis is based on archival optical and UV high-resolution spectra. We used Tlusty200/Synspec48 to compute line blanketed non-LTE model atmospheres and their corresponding synthetic spectra and derive the atmospheric parameters as well as the abundances of the most prominent elements. All stars have helium-dominated atmospheres with hardly any hydrogen and temperatures between 42000 K and 47000 K while their surface gravity spans between log g = 5.4 and 5.7. CD-31∘ 4800 shows an enrichment of nitrogen and the characteristic pattern of hydrogen burning via the CNO-cycle, while the rest of the elements have about the solar abundance. This points to the slow merger of two helium white dwarfs as the most likely origin for this system. The other three stars are enriched in carbon, nitrogen and neon while their intermediate mass element’s abundance scatters around the solar value. They were possibly formed in the deep mixing late hot flasher scenario.
Facultad de Ciencias Astronómicas y Geofísicas - Materia
-
Astronomía
subdwarfs
abundances
He-sdO
hot flasher
slow merger
atmospheric parameters
stellar atmospheres - Nivel de accesibilidad
- acceso abierto
- Condiciones de uso
- http://creativecommons.org/licenses/by-nc-nd/4.0/
- Repositorio
- Institución
- Universidad Nacional de La Plata
- OAI Identificador
- oai:sedici.unlp.edu.ar:10915/78622
Ver los metadatos del registro completo
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Chemical fingerprints of He-sdO starsSchindewolf, MarkusNémeth, PeterHeber, UlrichBattich, TiaraMiller Bertolami, Marcelo MiguelLatour, MarilynAstronomíasubdwarfsabundancesHe-sdOhot flasherslow mergeratmospheric parametersstellar atmospheresThe chemical composition of helium-rich hot subluminous O stars plays an important role to understand and model their formation history. We present a spectroscopic analysis of four He-sdO stars,CD-31∘ 4800, [CW83] 0904- 02, LSS 1274 and LS IV +10∘ 9. The analysis is based on archival optical and UV high-resolution spectra. We used Tlusty200/Synspec48 to compute line blanketed non-LTE model atmospheres and their corresponding synthetic spectra and derive the atmospheric parameters as well as the abundances of the most prominent elements. All stars have helium-dominated atmospheres with hardly any hydrogen and temperatures between 42000 K and 47000 K while their surface gravity spans between log g = 5.4 and 5.7. CD-31∘ 4800 shows an enrichment of nitrogen and the characteristic pattern of hydrogen burning via the CNO-cycle, while the rest of the elements have about the solar abundance. This points to the slow merger of two helium white dwarfs as the most likely origin for this system. The other three stars are enriched in carbon, nitrogen and neon while their intermediate mass element’s abundance scatters around the solar value. They were possibly formed in the deep mixing late hot flasher scenario.Facultad de Ciencias Astronómicas y Geofísicas2018-02info:eu-repo/semantics/articleinfo:eu-repo/semantics/publishedVersionArticulohttp://purl.org/coar/resource_type/c_6501info:ar-repo/semantics/articuloapplication/pdf27-34http://sedici.unlp.edu.ar/handle/10915/78622enginfo:eu-repo/semantics/altIdentifier/issn/2543-6376info:eu-repo/semantics/altIdentifier/doi/10.1515/astro-2018-0010info: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:UNLP2025-09-29T11:14:13Zoai:sedici.unlp.edu.ar:10915/78622Institucionalhttp://sedici.unlp.edu.ar/Universidad públicaNo correspondehttp://sedici.unlp.edu.ar/oai/snrdalira@sedici.unlp.edu.arArgentinaNo correspondeNo correspondeNo correspondeopendoar:13292025-09-29 11:14:13.793SEDICI (UNLP) - Universidad Nacional de La Platafalse |
dc.title.none.fl_str_mv |
Chemical fingerprints of He-sdO stars |
title |
Chemical fingerprints of He-sdO stars |
spellingShingle |
Chemical fingerprints of He-sdO stars Schindewolf, Markus Astronomía subdwarfs abundances He-sdO hot flasher slow merger atmospheric parameters stellar atmospheres |
title_short |
Chemical fingerprints of He-sdO stars |
title_full |
Chemical fingerprints of He-sdO stars |
title_fullStr |
Chemical fingerprints of He-sdO stars |
title_full_unstemmed |
Chemical fingerprints of He-sdO stars |
title_sort |
Chemical fingerprints of He-sdO stars |
dc.creator.none.fl_str_mv |
Schindewolf, Markus Németh, Peter Heber, Ulrich Battich, Tiara Miller Bertolami, Marcelo Miguel Latour, Marilyn |
author |
Schindewolf, Markus |
author_facet |
Schindewolf, Markus Németh, Peter Heber, Ulrich Battich, Tiara Miller Bertolami, Marcelo Miguel Latour, Marilyn |
author_role |
author |
author2 |
Németh, Peter Heber, Ulrich Battich, Tiara Miller Bertolami, Marcelo Miguel Latour, Marilyn |
author2_role |
author author author author author |
dc.subject.none.fl_str_mv |
Astronomía subdwarfs abundances He-sdO hot flasher slow merger atmospheric parameters stellar atmospheres |
topic |
Astronomía subdwarfs abundances He-sdO hot flasher slow merger atmospheric parameters stellar atmospheres |
dc.description.none.fl_txt_mv |
The chemical composition of helium-rich hot subluminous O stars plays an important role to understand and model their formation history. We present a spectroscopic analysis of four He-sdO stars,CD-31∘ 4800, [CW83] 0904- 02, LSS 1274 and LS IV +10∘ 9. The analysis is based on archival optical and UV high-resolution spectra. We used Tlusty200/Synspec48 to compute line blanketed non-LTE model atmospheres and their corresponding synthetic spectra and derive the atmospheric parameters as well as the abundances of the most prominent elements. All stars have helium-dominated atmospheres with hardly any hydrogen and temperatures between 42000 K and 47000 K while their surface gravity spans between log g = 5.4 and 5.7. CD-31∘ 4800 shows an enrichment of nitrogen and the characteristic pattern of hydrogen burning via the CNO-cycle, while the rest of the elements have about the solar abundance. This points to the slow merger of two helium white dwarfs as the most likely origin for this system. The other three stars are enriched in carbon, nitrogen and neon while their intermediate mass element’s abundance scatters around the solar value. They were possibly formed in the deep mixing late hot flasher scenario. Facultad de Ciencias Astronómicas y Geofísicas |
description |
The chemical composition of helium-rich hot subluminous O stars plays an important role to understand and model their formation history. We present a spectroscopic analysis of four He-sdO stars,CD-31∘ 4800, [CW83] 0904- 02, LSS 1274 and LS IV +10∘ 9. The analysis is based on archival optical and UV high-resolution spectra. We used Tlusty200/Synspec48 to compute line blanketed non-LTE model atmospheres and their corresponding synthetic spectra and derive the atmospheric parameters as well as the abundances of the most prominent elements. All stars have helium-dominated atmospheres with hardly any hydrogen and temperatures between 42000 K and 47000 K while their surface gravity spans between log g = 5.4 and 5.7. CD-31∘ 4800 shows an enrichment of nitrogen and the characteristic pattern of hydrogen burning via the CNO-cycle, while the rest of the elements have about the solar abundance. This points to the slow merger of two helium white dwarfs as the most likely origin for this system. The other three stars are enriched in carbon, nitrogen and neon while their intermediate mass element’s abundance scatters around the solar value. They were possibly formed in the deep mixing late hot flasher scenario. |
publishDate |
2018 |
dc.date.none.fl_str_mv |
2018-02 |
dc.type.none.fl_str_mv |
info:eu-repo/semantics/article info:eu-repo/semantics/publishedVersion Articulo 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://sedici.unlp.edu.ar/handle/10915/78622 |
url |
http://sedici.unlp.edu.ar/handle/10915/78622 |
dc.language.none.fl_str_mv |
eng |
language |
eng |
dc.relation.none.fl_str_mv |
info:eu-repo/semantics/altIdentifier/issn/2543-6376 info:eu-repo/semantics/altIdentifier/doi/10.1515/astro-2018-0010 |
dc.rights.none.fl_str_mv |
info:eu-repo/semantics/openAccess http://creativecommons.org/licenses/by-nc-nd/4.0/ Creative Commons Attribution-NonCommercial-NoDerivatives 4.0 International (CC BY-NC-ND 4.0) |
eu_rights_str_mv |
openAccess |
rights_invalid_str_mv |
http://creativecommons.org/licenses/by-nc-nd/4.0/ Creative Commons Attribution-NonCommercial-NoDerivatives 4.0 International (CC BY-NC-ND 4.0) |
dc.format.none.fl_str_mv |
application/pdf 27-34 |
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SEDICI (UNLP) - Universidad Nacional de La Plata |
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