Pulsational instabilities in hot pre-horizontal branch stars

Autores
Battich, Tiara; Miller Bertolami, Marcelo Miguel; Córsico, Alejandro Hugo; Althaus, Leandro Gabriel
Año de publicación
2017
Idioma
inglés
Tipo de recurso
artículo
Estado
versión publicada
Descripción
The ϵ mechanism is a self-excitation mechanism of pulsations which acts on the regions where nuclear burning takes place. It has been shown that the ϵ mechanism can excite pulsations in models of hot helium-core flash, and that the pulsations of LS IV-14° 116, a He-enriched hot subdwarf star, could be explained that way. We aim to study the ϵ mechanism effects on models of hot pre-horizontal branch stars and determine, if possible, a domain of instability in the log g - log Teff plane. We compute non-adiabatic non-radial pulsations on such stellar models, adopting different values of initial chemical abundances and mass of the hydrogen envelope at the time of the main helium flash. We find an instability domain of long-period (400 s ≤ P ≤ 2500 s) g-modes for models with 22000K ≤ Teff ≤ 50000K and 4.67 ≤ log g ≤ 6.15.
Facultad de Ciencias Astronómicas y Geofísicas
Instituto de Astrofísica de La Plata
Materia
Ciencias Astronómicas
Estrellas Celestiales
Nivel de accesibilidad
acceso abierto
Condiciones de uso
http://creativecommons.org/licenses/by-nc-sa/4.0/
Repositorio
SEDICI (UNLP)
Institución
Universidad Nacional de La Plata
OAI Identificador
oai:sedici.unlp.edu.ar:10915/87518
Acceder
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oai_identifier_str oai:sedici.unlp.edu.ar:10915/87518
network_acronym_str SEDICI
repository_id_str 1329
network_name_str SEDICI (UNLP)
spelling Pulsational instabilities in hot pre-horizontal branch starsBattich, TiaraMiller Bertolami, Marcelo MiguelCórsico, Alejandro HugoAlthaus, Leandro GabrielCiencias AstronómicasEstrellas CelestialesThe ϵ mechanism is a self-excitation mechanism of pulsations which acts on the regions where nuclear burning takes place. It has been shown that the ϵ mechanism can excite pulsations in models of hot helium-core flash, and that the pulsations of LS IV-14° 116, a He-enriched hot subdwarf star, could be explained that way. We aim to study the ϵ mechanism effects on models of hot pre-horizontal branch stars and determine, if possible, a domain of instability in the log g - log Teff plane. We compute non-adiabatic non-radial pulsations on such stellar models, adopting different values of initial chemical abundances and mass of the hydrogen envelope at the time of the main helium flash. We find an instability domain of long-period (400 s ≤ P ≤ 2500 s) g-modes for models with 22000K ≤ Teff ≤ 50000K and 4.67 ≤ log g ≤ 6.15.Facultad de Ciencias Astronómicas y GeofísicasInstituto de Astrofísica de La Plata2017info: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/10915/87518enginfo:eu-repo/semantics/altIdentifier/issn/2101-6275info:eu-repo/semantics/altIdentifier/doi/10.1051/epjconf/201715206010info: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:UNLP2025-09-29T11:17:13Zoai:sedici.unlp.edu.ar:10915/87518Institucionalhttp://sedici.unlp.edu.ar/Universidad públicaNo correspondehttp://sedici.unlp.edu.ar/oai/snrdalira@sedici.unlp.edu.arArgentinaNo correspondeNo correspondeNo correspondeopendoar:13292025-09-29 11:17:14.108SEDICI (UNLP) - Universidad Nacional de La Platafalse
dc.title.none.fl_str_mv Pulsational instabilities in hot pre-horizontal branch stars
title Pulsational instabilities in hot pre-horizontal branch stars
spellingShingle Pulsational instabilities in hot pre-horizontal branch stars
Battich, Tiara
Ciencias Astronómicas
Estrellas Celestiales
title_short Pulsational instabilities in hot pre-horizontal branch stars
title_full Pulsational instabilities in hot pre-horizontal branch stars
title_fullStr Pulsational instabilities in hot pre-horizontal branch stars
title_full_unstemmed Pulsational instabilities in hot pre-horizontal branch stars
title_sort Pulsational instabilities in hot pre-horizontal branch stars
dc.creator.none.fl_str_mv Battich, Tiara
Miller Bertolami, Marcelo Miguel
Córsico, Alejandro Hugo
Althaus, Leandro Gabriel
author Battich, Tiara
author_facet Battich, Tiara
Miller Bertolami, Marcelo Miguel
Córsico, Alejandro Hugo
Althaus, Leandro Gabriel
author_role author
author2 Miller Bertolami, Marcelo Miguel
Córsico, Alejandro Hugo
Althaus, Leandro Gabriel
author2_role author
author
author
dc.subject.none.fl_str_mv Ciencias Astronómicas
Estrellas Celestiales
topic Ciencias Astronómicas
Estrellas Celestiales
dc.description.none.fl_txt_mv The ϵ mechanism is a self-excitation mechanism of pulsations which acts on the regions where nuclear burning takes place. It has been shown that the ϵ mechanism can excite pulsations in models of hot helium-core flash, and that the pulsations of LS IV-14° 116, a He-enriched hot subdwarf star, could be explained that way. We aim to study the ϵ mechanism effects on models of hot pre-horizontal branch stars and determine, if possible, a domain of instability in the log g - log Teff plane. We compute non-adiabatic non-radial pulsations on such stellar models, adopting different values of initial chemical abundances and mass of the hydrogen envelope at the time of the main helium flash. We find an instability domain of long-period (400 s ≤ P ≤ 2500 s) g-modes for models with 22000K ≤ Teff ≤ 50000K and 4.67 ≤ log g ≤ 6.15.
Facultad de Ciencias Astronómicas y Geofísicas
Instituto de Astrofísica de La Plata
description The ϵ mechanism is a self-excitation mechanism of pulsations which acts on the regions where nuclear burning takes place. It has been shown that the ϵ mechanism can excite pulsations in models of hot helium-core flash, and that the pulsations of LS IV-14° 116, a He-enriched hot subdwarf star, could be explained that way. We aim to study the ϵ mechanism effects on models of hot pre-horizontal branch stars and determine, if possible, a domain of instability in the log g - log Teff plane. We compute non-adiabatic non-radial pulsations on such stellar models, adopting different values of initial chemical abundances and mass of the hydrogen envelope at the time of the main helium flash. We find an instability domain of long-period (400 s ≤ P ≤ 2500 s) g-modes for models with 22000K ≤ Teff ≤ 50000K and 4.67 ≤ log g ≤ 6.15.
publishDate 2017
dc.date.none.fl_str_mv 2017
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/10915/87518
url http://sedici.unlp.edu.ar/handle/10915/87518
dc.language.none.fl_str_mv eng
language eng
dc.relation.none.fl_str_mv info:eu-repo/semantics/altIdentifier/issn/2101-6275
info:eu-repo/semantics/altIdentifier/doi/10.1051/epjconf/201715206010
dc.rights.none.fl_str_mv info:eu-repo/semantics/openAccess
http://creativecommons.org/licenses/by-nc-sa/4.0/
Creative Commons Attribution-NonCommercial-ShareAlike 4.0 International (CC BY-NC-SA 4.0)
eu_rights_str_mv openAccess
rights_invalid_str_mv http://creativecommons.org/licenses/by-nc-sa/4.0/
Creative Commons Attribution-NonCommercial-ShareAlike 4.0 International (CC BY-NC-SA 4.0)
dc.format.none.fl_str_mv application/pdf
dc.source.none.fl_str_mv reponame:SEDICI (UNLP)
instname:Universidad Nacional de La Plata
instacron:UNLP
reponame_str SEDICI (UNLP)
collection SEDICI (UNLP)
instname_str Universidad Nacional de La Plata
instacron_str UNLP
institution UNLP
repository.name.fl_str_mv SEDICI (UNLP) - Universidad Nacional de La Plata
repository.mail.fl_str_mv alira@sedici.unlp.edu.ar
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