Hot DQ white dwarfs: a pulsational test of the mixing scenario for their formation

Hot DQ white dwarfs constitute a new class of white dwarf stars, uncovered recently within the framework of SDSS project. There exist nine of them, out of a total of several thousands white dwarfs spectroscopically identified. Recently, three hot DQ white dwarfs have been reported to exhibit photome...

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Detalles Bibliográficos
Autores principales: Romero, Alejandra Daniela, Córsico, Alejandro Hugo, Althaus, Leandro Gabriel, García Berro, Enrique
Formato: Articulo Comunicacion
Lenguaje:Inglés
Publicado: 2009
Materias:
Astronomía
Física
white dwarfs
photometric variability
Acceso en línea:http://sedici.unlp.edu.ar/handle/10915/138655
Aporte de:
SEDICI (UNLP) de Universidad Nacional de La Plata
id I19-R120-10915-138655
record_format dspace
institution Universidad Nacional de La Plata
institution_str I-19
repository_str R-120
collection SEDICI (UNLP)
language Inglés
topic Astronomía
Física
white dwarfs
photometric variability
spellingShingle Astronomía
Física
white dwarfs
photometric variability
Romero, Alejandra Daniela
Córsico, Alejandro Hugo
Althaus, Leandro Gabriel
García Berro, Enrique
Hot DQ white dwarfs: a pulsational test of the mixing scenario for their formation
topic_facet Astronomía
Física
white dwarfs
photometric variability
description Hot DQ white dwarfs constitute a new class of white dwarf stars, uncovered recently within the framework of SDSS project. There exist nine of them, out of a total of several thousands white dwarfs spectroscopically identified. Recently, three hot DQ white dwarfs have been reported to exhibit photometric variability with periods compatible with pulsation g -modes. In this contribution, we presented the results of a non-adiabatic pulsation analysis of the recently discovered carbon-rich hot DQ white dwarf stars. Our study relies on the full evolutionary models of hot DQ white dwarfs recently developed by Althaus et al . (2009), that consistently cover the whole evolution from the born-again stage to the white dwarf cooling track. Specifically, we performed a stability analysis on white dwarf models from stages before the blue edge of the DBV instability strip ( T eff ≈ 30000 K) until the domain of the hot DQ white dwarfs (18000-24000 K), including the transition DB→hot DQ white dwarf. We explore evolutionary models with M * = 0.585 M ⊙ and M * = 0.87 M ⊙ , and two values of thickness of the He-rich envelope ( M He = 2 × 10 −7 M * and M He = 10 −8 M * ).
format Articulo
Comunicacion
author Romero, Alejandra Daniela
Córsico, Alejandro Hugo
Althaus, Leandro Gabriel
García Berro, Enrique
author_facet Romero, Alejandra Daniela
Córsico, Alejandro Hugo
Althaus, Leandro Gabriel
García Berro, Enrique
author_sort Romero, Alejandra Daniela
title Hot DQ white dwarfs: a pulsational test of the mixing scenario for their formation
title_short Hot DQ white dwarfs: a pulsational test of the mixing scenario for their formation
title_full Hot DQ white dwarfs: a pulsational test of the mixing scenario for their formation
title_fullStr Hot DQ white dwarfs: a pulsational test of the mixing scenario for their formation
title_full_unstemmed Hot DQ white dwarfs: a pulsational test of the mixing scenario for their formation
title_sort hot dq white dwarfs: a pulsational test of the mixing scenario for their formation
publishDate 2009
url http://sedici.unlp.edu.ar/handle/10915/138655
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AT althausleandrogabriel hotdqwhitedwarfsapulsationaltestofthemixingscenariofortheirformation
AT garciaberroenrique hotdqwhitedwarfsapulsationaltestofthemixingscenariofortheirformation
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