New evolutionary models for massive ZZ Ceti stars, I : first results for their pulsational properties

Autores
Althaus, Leandro Gabriel; Serenelli, A. M.; Corsico, Alejandro Hugo; Montgomery, M. H.
Año de publicación
2003
Idioma
inglés
Tipo de recurso
artículo
Estado
versión publicada
Descripción
Chaotic orbits suffer significant changes as a result of small perturbations. One can thus wonder whether the dynamical friction suffered by a satellite on a regular orbit, and interacting with the stars of a galaxy, will be different if the bulk of the stars of the galaxy are in regular or chaotic orbits. In order to check that idea, we investigated the orbital decay (caused by dynamical friction) of a rigid satellite moving within a larger stellar system (a galaxy) whose potential is nonintegrable. We performed numerical experiments using two kinds of triaxial galaxy models: (1) the triaxial generalization of Dehnen's spherical mass model (Dehnen; Merritt & Fridman); (2) a modified Satoh model (Satoh; Carpintero, Muzzio, & Wachlin). The percentages of chaotic orbits present in these models were increased by perturbing them. In the first case, a central compact object (black hole) was introduced; in the second case, the perturbation was produced by allowing the galaxy to move on a circular orbit in a logarithmic potential. The equations of motion were integrated with a non-self-consistent code. Our results show that the presence of chaotic orbits does not affect significantly the orbital decay of the satellite.
Fil: Althaus, Leandro Gabriel. Universidad Nacional de la Plata. Facultad de Ciencias Astronómicas y Geofísicas; Argentina
Fil: Serenelli, A. M.. Universidad Nacional de la Plata. Facultad de Ciencias Astronómicas y Geofísicas; Argentina
Fil: Corsico, Alejandro Hugo. Universidad Nacional de la Plata. Facultad de Ciencias Astronómicas y Geofísicas; Argentina
Fil: Montgomery, M. H.. Institute of Astronomy; Reino Unido
Materia
Evolution of stars
Abundances
Interior stars
White dwarfs
Oscillations of stars
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:11336/37095
Acceder
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network_acronym_str CONICETDig
repository_id_str 3498
network_name_str CONICET Digital (CONICET)
spelling New evolutionary models for massive ZZ Ceti stars, I : first results for their pulsational propertiesAlthaus, Leandro GabrielSerenelli, A. M.Corsico, Alejandro HugoMontgomery, M. H.Evolution of starsAbundancesInterior starsWhite dwarfsOscillations of starshttps://purl.org/becyt/ford/1.3https://purl.org/becyt/ford/1Chaotic orbits suffer significant changes as a result of small perturbations. One can thus wonder whether the dynamical friction suffered by a satellite on a regular orbit, and interacting with the stars of a galaxy, will be different if the bulk of the stars of the galaxy are in regular or chaotic orbits. In order to check that idea, we investigated the orbital decay (caused by dynamical friction) of a rigid satellite moving within a larger stellar system (a galaxy) whose potential is nonintegrable. We performed numerical experiments using two kinds of triaxial galaxy models: (1) the triaxial generalization of Dehnen's spherical mass model (Dehnen; Merritt & Fridman); (2) a modified Satoh model (Satoh; Carpintero, Muzzio, & Wachlin). The percentages of chaotic orbits present in these models were increased by perturbing them. In the first case, a central compact object (black hole) was introduced; in the second case, the perturbation was produced by allowing the galaxy to move on a circular orbit in a logarithmic potential. The equations of motion were integrated with a non-self-consistent code. Our results show that the presence of chaotic orbits does not affect significantly the orbital decay of the satellite.Fil: Althaus, Leandro Gabriel. Universidad Nacional de la Plata. Facultad de Ciencias Astronómicas y Geofísicas; ArgentinaFil: Serenelli, A. M.. Universidad Nacional de la Plata. Facultad de Ciencias Astronómicas y Geofísicas; ArgentinaFil: Corsico, Alejandro Hugo. Universidad Nacional de la Plata. Facultad de Ciencias Astronómicas y Geofísicas; ArgentinaFil: Montgomery, M. H.. Institute of Astronomy; Reino UnidoEDP Sciences2003-06info:eu-repo/semantics/articleinfo:eu-repo/semantics/publishedVersionhttp://purl.org/coar/resource_type/c_6501info:ar-repo/semantics/articuloapplication/pdfapplication/pdfapplication/pdfhttp://hdl.handle.net/11336/37095Althaus, Leandro Gabriel; Serenelli, A. M.; Corsico, Alejandro Hugo; Montgomery, M. H.; New evolutionary models for massive ZZ Ceti stars, I : first results for their pulsational properties; EDP Sciences; Astronomy and Astrophysics; 404; 6-2003; 593-6090004-6361CONICET DigitalCONICETenginfo:eu-repo/semantics/altIdentifier/doi/10.1051/0004-6361:20030472info:eu-repo/semantics/altIdentifier/url/https://www.aanda.org/articles/aa/abs/2003/23/aah4325/aah4325.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 Técnicas2025-09-29T10:11:11Zoai:ri.conicet.gov.ar:11336/37095instacron: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 10:11:12.252CONICET Digital (CONICET) - Consejo Nacional de Investigaciones Científicas y Técnicasfalse
dc.title.none.fl_str_mv New evolutionary models for massive ZZ Ceti stars, I : first results for their pulsational properties
title New evolutionary models for massive ZZ Ceti stars, I : first results for their pulsational properties
spellingShingle New evolutionary models for massive ZZ Ceti stars, I : first results for their pulsational properties
Althaus, Leandro Gabriel
Evolution of stars
Abundances
Interior stars
White dwarfs
Oscillations of stars
title_short New evolutionary models for massive ZZ Ceti stars, I : first results for their pulsational properties
title_full New evolutionary models for massive ZZ Ceti stars, I : first results for their pulsational properties
title_fullStr New evolutionary models for massive ZZ Ceti stars, I : first results for their pulsational properties
title_full_unstemmed New evolutionary models for massive ZZ Ceti stars, I : first results for their pulsational properties
title_sort New evolutionary models for massive ZZ Ceti stars, I : first results for their pulsational properties
dc.creator.none.fl_str_mv Althaus, Leandro Gabriel
Serenelli, A. M.
Corsico, Alejandro Hugo
Montgomery, M. H.
author Althaus, Leandro Gabriel
author_facet Althaus, Leandro Gabriel
Serenelli, A. M.
Corsico, Alejandro Hugo
Montgomery, M. H.
author_role author
author2 Serenelli, A. M.
Corsico, Alejandro Hugo
Montgomery, M. H.
author2_role author
author
author
dc.subject.none.fl_str_mv Evolution of stars
Abundances
Interior stars
White dwarfs
Oscillations of stars
topic Evolution of stars
Abundances
Interior stars
White dwarfs
Oscillations of stars
purl_subject.fl_str_mv https://purl.org/becyt/ford/1.3
https://purl.org/becyt/ford/1
dc.description.none.fl_txt_mv Chaotic orbits suffer significant changes as a result of small perturbations. One can thus wonder whether the dynamical friction suffered by a satellite on a regular orbit, and interacting with the stars of a galaxy, will be different if the bulk of the stars of the galaxy are in regular or chaotic orbits. In order to check that idea, we investigated the orbital decay (caused by dynamical friction) of a rigid satellite moving within a larger stellar system (a galaxy) whose potential is nonintegrable. We performed numerical experiments using two kinds of triaxial galaxy models: (1) the triaxial generalization of Dehnen's spherical mass model (Dehnen; Merritt & Fridman); (2) a modified Satoh model (Satoh; Carpintero, Muzzio, & Wachlin). The percentages of chaotic orbits present in these models were increased by perturbing them. In the first case, a central compact object (black hole) was introduced; in the second case, the perturbation was produced by allowing the galaxy to move on a circular orbit in a logarithmic potential. The equations of motion were integrated with a non-self-consistent code. Our results show that the presence of chaotic orbits does not affect significantly the orbital decay of the satellite.
Fil: Althaus, Leandro Gabriel. Universidad Nacional de la Plata. Facultad de Ciencias Astronómicas y Geofísicas; Argentina
Fil: Serenelli, A. M.. Universidad Nacional de la Plata. Facultad de Ciencias Astronómicas y Geofísicas; Argentina
Fil: Corsico, Alejandro Hugo. Universidad Nacional de la Plata. Facultad de Ciencias Astronómicas y Geofísicas; Argentina
Fil: Montgomery, M. H.. Institute of Astronomy; Reino Unido
description Chaotic orbits suffer significant changes as a result of small perturbations. One can thus wonder whether the dynamical friction suffered by a satellite on a regular orbit, and interacting with the stars of a galaxy, will be different if the bulk of the stars of the galaxy are in regular or chaotic orbits. In order to check that idea, we investigated the orbital decay (caused by dynamical friction) of a rigid satellite moving within a larger stellar system (a galaxy) whose potential is nonintegrable. We performed numerical experiments using two kinds of triaxial galaxy models: (1) the triaxial generalization of Dehnen's spherical mass model (Dehnen; Merritt & Fridman); (2) a modified Satoh model (Satoh; Carpintero, Muzzio, & Wachlin). The percentages of chaotic orbits present in these models were increased by perturbing them. In the first case, a central compact object (black hole) was introduced; in the second case, the perturbation was produced by allowing the galaxy to move on a circular orbit in a logarithmic potential. The equations of motion were integrated with a non-self-consistent code. Our results show that the presence of chaotic orbits does not affect significantly the orbital decay of the satellite.
publishDate 2003
dc.date.none.fl_str_mv 2003-06
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/11336/37095
Althaus, Leandro Gabriel; Serenelli, A. M.; Corsico, Alejandro Hugo; Montgomery, M. H.; New evolutionary models for massive ZZ Ceti stars, I : first results for their pulsational properties; EDP Sciences; Astronomy and Astrophysics; 404; 6-2003; 593-609
0004-6361
CONICET Digital
CONICET
url http://hdl.handle.net/11336/37095
identifier_str_mv Althaus, Leandro Gabriel; Serenelli, A. M.; Corsico, Alejandro Hugo; Montgomery, M. H.; New evolutionary models for massive ZZ Ceti stars, I : first results for their pulsational properties; EDP Sciences; Astronomy and Astrophysics; 404; 6-2003; 593-609
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/10.1051/0004-6361:20030472
info:eu-repo/semantics/altIdentifier/url/https://www.aanda.org/articles/aa/abs/2003/23/aah4325/aah4325.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
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 13.070432

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