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dc.contributor.author
Corsico, Alejandro Hugo  
dc.contributor.author
Romero, Alejandra Daniela  
dc.contributor.author
Althaus, Leandro Gabriel  
dc.contributor.author
Hermes, J. J.  
dc.date.available
2019-08-29T14:48:26Z  
dc.date.issued
2012-11  
dc.identifier.citation
Corsico, Alejandro Hugo; Romero, Alejandra Daniela; Althaus, Leandro Gabriel; Hermes, J. J.; The seismic properties of low-mass He-core white dwarf stars; EDP Sciences; Astronomy and Astrophysics; 547; 11-2012; 96-109  
dc.identifier.issn
0004-6361  
dc.identifier.uri
http://hdl.handle.net/11336/82476  
dc.description.abstract
Context. In recent years, many low-mass (≲ 0.45 M ·) white dwarf stars expected to harbor He cores have been detected in the field of the Milky Way and in several galactic globular and open clusters. Until recently, no objects of this kind showed pulsations. This situation has changed recently with the exciting discovery of SDSS J184037.78+642312.3, the first pulsating low-mass white dwarf star. Aims. Motivated by this extremely important finding, and in view of the very valuable asteroseismological potential of these objects, we present here a detailed pulsational study applied to low-mass He-core white dwarfs with masses ranging from 0.17 to 0.46 M ·, based on full evolutionary models representative of these objects. This study is aimed to provide a theoretical basis from which to interpret future observations of variable low-mass white dwarfs. Methods. The background stellar models on which our pulsational analysis was carried out were derived by taking into account the complete evolutionary history of the progenitor stars, with special emphasis on the diffusion processes acting during the white dwarf cooling phase. We computed nonradial g-modes to assess the dependence of the pulsational properties of these objects with stellar parameters such as the stellar mass and the effective temperature, and also with element diffusion processes. We also performed a g-and p-mode pulsational stability analysis on our models and found well-defined blue edges of the instability domain, where these stars should start to exhibit pulsations. Results. We found substantial differences in the seismic properties of white dwarfs with M * ≳ 0.20 M · and the extremely low-mass (ELM) white dwarfs (M * ≲ 0.20 M ·). Specifically, g-mode pulsation modes in ELM white dwarfs mainly probe the core regions and are not dramatically affected by mode-trapping effects by the He/H interface, whereas the opposite is true for more massive He-core white dwarfs. We found that element diffusion processes substantially affects the shape of the He/H chemical transition region, leading to non-negligible changes in the period spectrum of low-mass white dwarfs, in particular in the range of stellar masses characteristic of ELM objects. Finally, our stability analysis successfully predicts the pulsations of the only known variable low-mass white dwarf (SDSS J184037.78+642312.3) at the right effective temperature, stellar mass and range of periods. Conclusions. Our computations predict both g-and p-mode pulsational instabilities in a significant number of known low-mass and ELM white dwarfs. It is worth observing these stars in order to discover if they pulsate.  
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
Asteroseismology  
dc.subject
Stars: Evolution  
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Stars: Interiors  
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Stars: Oscillations  
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White Dwarfs  
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Astronomía  
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Ciencias Físicas  
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CIENCIAS NATURALES Y EXACTAS  
dc.title
The seismic properties of low-mass He-core white dwarf 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
2019-08-23T17:43:01Z  
dc.journal.volume
547  
dc.journal.pagination
96-109  
dc.journal.pais
Francia  
dc.journal.ciudad
Paris  
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  
dc.description.fil
Fil: Romero, Alejandra Daniela. 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  
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  
dc.description.fil
Fil: Hermes, J. J.. University of Texas at Austin; Estados Unidos  
dc.journal.title
Astronomy and Astrophysics  
dc.relation.alternativeid
info:eu-repo/semantics/altIdentifier/doi/http://dx.doi.org/10.1051/0004-6361/201220114  
dc.relation.alternativeid
info:eu-repo/semantics/altIdentifier/url/https://www.aanda.org/articles/aa/abs/2012/11/aa20114-12/aa20114-12.html