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
- Institución
- Consejo Nacional de Investigaciones Científicas y Técnicas
- OAI Identificador
- oai:ri.conicet.gov.ar:11336/82488
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oai:ri.conicet.gov.ar:11336/82488 |
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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 Técnicas2025-09-29T09:50:22Zoai: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:34982025-09-29 09:50:23.124CONICET 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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1844613552772481024 |
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13.070432 |