Pulsational instabilities driven by the mechanism in hot pre-horizontal branch stars: I. the hot-flasher scenario

Autores
Battich, Tiara; Miller Bertolami, Marcelo Miguel; Corsico, Alejandro Hugo; Althaus, Leandro Gabriel
Año de publicación
2018
Idioma
inglés
Tipo de recurso
artículo
Estado
versión publicada
Descripción
Context. The mechanism is a self-excitation mechanism of stellar pulsations that acts in regions inside the star where nuclear burning takes place. It has been shown that the mechanism can excite pulsations in models of hot pre-horizontal branch stars before they settle into the stable helium core-burning phase. Moreover, it has been shown that this mechanism could explain the shortest periods of LS IV-14°116, a mild He-sdBV star. Aims. We aim to study the mechanism in stellar models appropriate for hot pre-horizontal branch stars to predict their pulsational properties and the instability domain in the log g - log Te ff plane. Methods. We performed detailed computations of non-adiabatic non-radial pulsations on stellar models during the helium subflashes just before the helium-core burning phase. Computations were carried out for different values of initial helium composition, metallicity, and envelope mass at the moment of helium flash. Results. We find an instability domain of long-period gravity modes due to the mechanism in the log g - log Te ff plane at roughly 22 000 KTe ff50 000 K and 4.67log g6.15. Consequently, we find instabilities due to the mechanism on pre-extreme horizontal branch stellar models (Te ff 22 000 K), but not on pre-blue horizontal branch stellar models (Te ff21 000 K). The periods of excited modes range between 200 and ~2000 s. Comparison with the three known pulsating He-rich subdwarfs shows that mechanism can excite gravity modes in stars with similar surface properties (He abundances, log g, log Te ff), but in our models it is only able to excite modes in the range of the shortest observed periods. Conclusions. We predict a new instability strip for hot-subdwarf stars of which LS IV-14°116 could be the first inhabitant. Based on simple estimates we expect 1 to 10 stars in the current samples of hot-subdwarf stars to be pulsating by the mechanism. Our results could constitute a theoretical basis for future searches of pulsators in the Galactic field.
Fil: Battich, Tiara. 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: Miller Bertolami, Marcelo Miguel. 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: Corsico, Alejandro Hugo. 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: Althaus, Leandro Gabriel. 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
ASTEROSEISMOLOGY
STARS: HORIZONTAL-BRANCH
STARS: INTERIORS
STARS: LOW-MASS
STARS: OSCILLATIONS
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:11336/82488
Acceder
id CONICETDig_81ced8fa0c228d7dbed7dc7c912ef7bb
oai_identifier_str oai:ri.conicet.gov.ar:11336/82488
network_acronym_str CONICETDig
repository_id_str 3498
network_name_str CONICET Digital (CONICET)
spelling Pulsational instabilities driven by the mechanism in hot pre-horizontal branch stars: I. the hot-flasher scenarioBattich, TiaraMiller Bertolami, Marcelo MiguelCorsico, Alejandro HugoAlthaus, Leandro GabrielASTEROSEISMOLOGYSTARS: HORIZONTAL-BRANCHSTARS: INTERIORSSTARS: LOW-MASSSTARS: OSCILLATIONShttps://purl.org/becyt/ford/1.3https://purl.org/becyt/ford/1Context. The mechanism is a self-excitation mechanism of stellar pulsations that acts in regions inside the star where nuclear burning takes place. It has been shown that the mechanism can excite pulsations in models of hot pre-horizontal branch stars before they settle into the stable helium core-burning phase. Moreover, it has been shown that this mechanism could explain the shortest periods of LS IV-14°116, a mild He-sdBV star. Aims. We aim to study the mechanism in stellar models appropriate for hot pre-horizontal branch stars to predict their pulsational properties and the instability domain in the log g - log Te ff plane. Methods. We performed detailed computations of non-adiabatic non-radial pulsations on stellar models during the helium subflashes just before the helium-core burning phase. Computations were carried out for different values of initial helium composition, metallicity, and envelope mass at the moment of helium flash. Results. We find an instability domain of long-period gravity modes due to the mechanism in the log g - log Te ff plane at roughly 22 000 KTe ff50 000 K and 4.67log g6.15. Consequently, we find instabilities due to the mechanism on pre-extreme horizontal branch stellar models (Te ff 22 000 K), but not on pre-blue horizontal branch stellar models (Te ff21 000 K). The periods of excited modes range between 200 and ~2000 s. Comparison with the three known pulsating He-rich subdwarfs shows that mechanism can excite gravity modes in stars with similar surface properties (He abundances, log g, log Te ff), but in our models it is only able to excite modes in the range of the shortest observed periods. Conclusions. We predict a new instability strip for hot-subdwarf stars of which LS IV-14°116 could be the first inhabitant. Based on simple estimates we expect 1 to 10 stars in the current samples of hot-subdwarf stars to be pulsating by the mechanism. Our results could constitute a theoretical basis for future searches of pulsators in the Galactic field.Fil: Battich, Tiara. 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: Miller Bertolami, Marcelo Miguel. 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: Corsico, Alejandro Hugo. 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: Althaus, Leandro Gabriel. 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; ArgentinaEDP Sciences2018-06info:eu-repo/semantics/articleinfo:eu-repo/semantics/publishedVersionhttp://purl.org/coar/resource_type/c_6501info:ar-repo/semantics/articuloapplication/pdfapplication/pdfapplication/pdfapplication/pdfapplication/pdfhttp://hdl.handle.net/11336/82488Battich, Tiara; Miller Bertolami, Marcelo Miguel; Corsico, Alejandro Hugo; Althaus, Leandro Gabriel; Pulsational instabilities driven by the mechanism in hot pre-horizontal branch stars: I. the hot-flasher scenario; EDP Sciences; Astronomy and Astrophysics; 614; 6-2018; 1-130004-6361CONICET DigitalCONICETenginfo:eu-repo/semantics/altIdentifier/doi/10.1051/0004-6361/201731463info:eu-repo/semantics/altIdentifier/url/https://www.aanda.org/articles/aa/abs/2018/06/aa31463-17/aa31463-17.htmlinfo:eu-repo/semantics/openAccesshttps://creativecommons.org/licenses/by-nc-sa/2.5/ar/reponame:CONICET Digital (CONICET)instname:Consejo Nacional de Investigaciones Científicas y Técnicas2025-10-22T11:19:43Zoai:ri.conicet.gov.ar:11336/82488instacron: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:34982025-10-22 11:19:43.392CONICET Digital (CONICET) - Consejo Nacional de Investigaciones Científicas y Técnicasfalse
dc.title.none.fl_str_mv Pulsational instabilities driven by the mechanism in hot pre-horizontal branch stars: I. the hot-flasher scenario
title Pulsational instabilities driven by the mechanism in hot pre-horizontal branch stars: I. the hot-flasher scenario
spellingShingle Pulsational instabilities driven by the mechanism in hot pre-horizontal branch stars: I. the hot-flasher scenario
Battich, Tiara
ASTEROSEISMOLOGY
STARS: HORIZONTAL-BRANCH
STARS: INTERIORS
STARS: LOW-MASS
STARS: OSCILLATIONS
title_short Pulsational instabilities driven by the mechanism in hot pre-horizontal branch stars: I. the hot-flasher scenario
title_full Pulsational instabilities driven by the mechanism in hot pre-horizontal branch stars: I. the hot-flasher scenario
title_fullStr Pulsational instabilities driven by the mechanism in hot pre-horizontal branch stars: I. the hot-flasher scenario
title_full_unstemmed Pulsational instabilities driven by the mechanism in hot pre-horizontal branch stars: I. the hot-flasher scenario
title_sort Pulsational instabilities driven by the mechanism in hot pre-horizontal branch stars: I. the hot-flasher scenario
dc.creator.none.fl_str_mv Battich, Tiara
Miller Bertolami, Marcelo Miguel
Corsico, Alejandro Hugo
Althaus, Leandro Gabriel
author Battich, Tiara
author_facet Battich, Tiara
Miller Bertolami, Marcelo Miguel
Corsico, Alejandro Hugo
Althaus, Leandro Gabriel
author_role author
author2 Miller Bertolami, Marcelo Miguel
Corsico, Alejandro Hugo
Althaus, Leandro Gabriel
author2_role author
author
author
dc.subject.none.fl_str_mv ASTEROSEISMOLOGY
STARS: HORIZONTAL-BRANCH
STARS: INTERIORS
STARS: LOW-MASS
STARS: OSCILLATIONS
topic ASTEROSEISMOLOGY
STARS: HORIZONTAL-BRANCH
STARS: INTERIORS
STARS: LOW-MASS
STARS: OSCILLATIONS
purl_subject.fl_str_mv https://purl.org/becyt/ford/1.3
https://purl.org/becyt/ford/1
dc.description.none.fl_txt_mv Context. The mechanism is a self-excitation mechanism of stellar pulsations that acts in regions inside the star where nuclear burning takes place. It has been shown that the mechanism can excite pulsations in models of hot pre-horizontal branch stars before they settle into the stable helium core-burning phase. Moreover, it has been shown that this mechanism could explain the shortest periods of LS IV-14°116, a mild He-sdBV star. Aims. We aim to study the mechanism in stellar models appropriate for hot pre-horizontal branch stars to predict their pulsational properties and the instability domain in the log g - log Te ff plane. Methods. We performed detailed computations of non-adiabatic non-radial pulsations on stellar models during the helium subflashes just before the helium-core burning phase. Computations were carried out for different values of initial helium composition, metallicity, and envelope mass at the moment of helium flash. Results. We find an instability domain of long-period gravity modes due to the mechanism in the log g - log Te ff plane at roughly 22 000 KTe ff50 000 K and 4.67log g6.15. Consequently, we find instabilities due to the mechanism on pre-extreme horizontal branch stellar models (Te ff 22 000 K), but not on pre-blue horizontal branch stellar models (Te ff21 000 K). The periods of excited modes range between 200 and ~2000 s. Comparison with the three known pulsating He-rich subdwarfs shows that mechanism can excite gravity modes in stars with similar surface properties (He abundances, log g, log Te ff), but in our models it is only able to excite modes in the range of the shortest observed periods. Conclusions. We predict a new instability strip for hot-subdwarf stars of which LS IV-14°116 could be the first inhabitant. Based on simple estimates we expect 1 to 10 stars in the current samples of hot-subdwarf stars to be pulsating by the mechanism. Our results could constitute a theoretical basis for future searches of pulsators in the Galactic field.
Fil: Battich, Tiara. 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: Miller Bertolami, Marcelo Miguel. 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: Corsico, Alejandro Hugo. 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: Althaus, Leandro Gabriel. 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 Context. The mechanism is a self-excitation mechanism of stellar pulsations that acts in regions inside the star where nuclear burning takes place. It has been shown that the mechanism can excite pulsations in models of hot pre-horizontal branch stars before they settle into the stable helium core-burning phase. Moreover, it has been shown that this mechanism could explain the shortest periods of LS IV-14°116, a mild He-sdBV star. Aims. We aim to study the mechanism in stellar models appropriate for hot pre-horizontal branch stars to predict their pulsational properties and the instability domain in the log g - log Te ff plane. Methods. We performed detailed computations of non-adiabatic non-radial pulsations on stellar models during the helium subflashes just before the helium-core burning phase. Computations were carried out for different values of initial helium composition, metallicity, and envelope mass at the moment of helium flash. Results. We find an instability domain of long-period gravity modes due to the mechanism in the log g - log Te ff plane at roughly 22 000 KTe ff50 000 K and 4.67log g6.15. Consequently, we find instabilities due to the mechanism on pre-extreme horizontal branch stellar models (Te ff 22 000 K), but not on pre-blue horizontal branch stellar models (Te ff21 000 K). The periods of excited modes range between 200 and ~2000 s. Comparison with the three known pulsating He-rich subdwarfs shows that mechanism can excite gravity modes in stars with similar surface properties (He abundances, log g, log Te ff), but in our models it is only able to excite modes in the range of the shortest observed periods. Conclusions. We predict a new instability strip for hot-subdwarf stars of which LS IV-14°116 could be the first inhabitant. Based on simple estimates we expect 1 to 10 stars in the current samples of hot-subdwarf stars to be pulsating by the mechanism. Our results could constitute a theoretical basis for future searches of pulsators in the Galactic field.
publishDate 2018
dc.date.none.fl_str_mv 2018-06
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/11336/82488
Battich, Tiara; Miller Bertolami, Marcelo Miguel; Corsico, Alejandro Hugo; Althaus, Leandro Gabriel; Pulsational instabilities driven by the mechanism in hot pre-horizontal branch stars: I. the hot-flasher scenario; EDP Sciences; Astronomy and Astrophysics; 614; 6-2018; 1-13
0004-6361
CONICET Digital
CONICET
url http://hdl.handle.net/11336/82488
identifier_str_mv Battich, Tiara; Miller Bertolami, Marcelo Miguel; Corsico, Alejandro Hugo; Althaus, Leandro Gabriel; Pulsational instabilities driven by the mechanism in hot pre-horizontal branch stars: I. the hot-flasher scenario; EDP Sciences; Astronomy and Astrophysics; 614; 6-2018; 1-13
0004-6361
CONICET Digital
CONICET
dc.language.none.fl_str_mv eng
language eng
dc.relation.none.fl_str_mv info:eu-repo/semantics/altIdentifier/doi/10.1051/0004-6361/201731463
info:eu-repo/semantics/altIdentifier/url/https://www.aanda.org/articles/aa/abs/2018/06/aa31463-17/aa31463-17.html
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
application/pdf
application/pdf
application/pdf
dc.publisher.none.fl_str_mv EDP Sciences
publisher.none.fl_str_mv EDP Sciences
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 12.982451

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