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dc.contributor.author Althaus, Leandro Gabriel
dc.contributor.author de Gerónimo, Francisco César
dc.contributor.author Corsico, Alejandro Hugo
dc.contributor.author Torres, Santiago
dc.contributor.author García Berro, Enrique
dc.date.available 2018-04-06T14:03:19Z
dc.date.issued 2017-01
dc.identifier.citation Althaus, Leandro Gabriel; de Gerónimo, Francisco César; Corsico, Alejandro Hugo; Torres, Santiago; García Berro, Enrique; The evolution of white dwarfs resulting from helium-enhanced, low-metallicity progenitor stars; EDP Sciences; Astronomy and Astrophysics; 597; 1-2017; A67
dc.identifier.issn 0004-6361
dc.identifier.uri http://hdl.handle.net/11336/41060
dc.description.abstract Context. Some globular clusters host multiple stellar populations with different chemical abundance patterns. This is particularly true for ω Centauri, which shows clear evidence of a helium-enriched subpopulation characterized by a helium abundance as high as Y = 0.4Aims. We present a whole and consistent set of evolutionary tracks from the ZAMS to the white dwarf stage that is appropriate for the study of the formation and evolution of white dwarfs resulting from the evolution of helium-rich progenitors.Methods. We derived white dwarf sequences from progenitors with stellar mass ranging from 0.60 to 2.0 M⊙ and for an initial helium abundance of Y = 0.4. We adopted two values of metallicity: Z = 0.001 and Z = 0.0005.Results. We explored different issues of white dwarf evolution and their helium-rich progenitors. In particular, the final mass of the remnants, the role of overshooting during the thermally pulsing phase, and the cooling of the resulting white dwarfs differ markedly from the evolutionary predictions of progenitor stars with the standard initial helium abundance. Finally, the pulsational properties of the resulting white dwarfs are also explored.Conclusions. We find that, for the range of initial masses explored in this paper, the final mass of the helium-rich progenitors is markedly higher than the final mass expected from progenitors with the usual helium abundance. We also find that progenitors with initial mass lower than M ≃ 0.65 M⊙ evolve directly into helium-core white dwarfs in less than 14 Gyr, and that, for larger progenitor masses, the evolution of the resulting low-mass carbon-oxygen white dwarfs is dominated by residual nuclear burning. For helium-core white dwarfs, we find that they evolve markedly faster than their counterparts coming from standard progenitors. Also, in contrast with what occurs for white dwarfs resulting from progenitors with the standard helium abundance, the impact of residual burning on the cooling time of white dwarfs is not affected by the occurrence of overshooting during the thermally pulsing phase of progenitor stars.
dc.format application/pdf
dc.language.iso eng
dc.publisher EDP Sciences
dc.rights info:eu-repo/semantics/openAccess
dc.rights.uri https://creativecommons.org/licenses/by-nc-sa/2.5/ar/
dc.subject Evolution of stars
dc.subject Interior stars
dc.subject White dwarfs
dc.subject.classification Astronomía
dc.subject.classification Ciencias Físicas
dc.subject.classification CIENCIAS NATURALES Y EXACTAS
dc.title The evolution of white dwarfs resulting from helium-enhanced, low-metallicity progenitor stars
dc.type info:eu-repo/semantics/article
dc.type info:ar-repo/semantics/artículo
dc.type info:eu-repo/semantics/publishedVersion
dc.date.updated 2018-03-26T14:37:55Z
dc.journal.volume 597
dc.journal.pagination A67
dc.journal.pais Francia
dc.journal.ciudad Paris
dc.description.fil 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. Universidad Nacional de La Plata. Facultad de Ciencias Astronómicas y Geofísicas; Argentina
dc.description.fil Fil: de Gerónimo, Francisco César. 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. Universidad Nacional de La Plata. Facultad de Ciencias Astronómicas y Geofísicas; Argentina
dc.description.fil 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. Universidad Nacional de La Plata. Facultad de Ciencias Astronómicas y Geofísicas; Argentina
dc.description.fil Fil: Torres, Santiago. Universidad Politécnica de Catalunya. Departament de Física Enginyeria; España
dc.description.fil Fil: García Berro, Enrique. Universidad Politécnica de Catalunya. Departament de Física Enginyeria; España
dc.journal.title Astronomy and Astrophysics
dc.relation.alternativeid info:eu-repo/semantics/altIdentifier/doi/http://dx.doi.org/10.1051/0004-6361/201629909
dc.relation.alternativeid info:eu-repo/semantics/altIdentifier/url/https://www.aanda.org/articles/aa/abs/2017/01/aa29909-16/aa29909-16.html
dc.conicet.fuente individual


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info:eu-repo/semantics/openAccess Excepto donde se diga explícitamente, este item se publica bajo la siguiente descripción: Creative Commons Attribution-NonCommercial-ShareAlike 2.5 Unported (CC BY-NC-SA 2.5)