EDP Sciences
Free Access
Volume 427, Number 3, December I 2004
Page(s) 923 - 932
Section Stellar structure and evolution
DOI https://doi.org/10.1051/0004-6361:20040416

A&A 427, 923-932 (2004)
DOI: 10.1051/0004-6361:20040416

Pulsations of massive ZZ Ceti stars with carbon/oxygen and oxygen/neon cores

A. H. Córsico1, 2, E. García-Berro3, 4, L. G. Althaus1, 2, 3 and J. Isern3, 5

1  Facultad de Ciencias Astronómicas y Geofísicas, Universidad Nacional de La Plata, Paseo del Bosque, s/n, (1900) La Plata, Argentina
    e-mail: [acorsico;althaus]@fcaglp.unlp.edu.ar
2  Instituto de Astrofísica La Plata, IALP, CONICET, Argentina
3  Departament de Física Aplicada, Universitat Politècnica de Catalunya, Av. del Canal Olímpic, s/n, 08860 Castelldefels, Spain
    e-mail: garcia@fa.upc.es;isern@ieec.fcr.es
4  Institut d'Estudis Espacials de Catalunya, Ed. Nexus, c/Gran Capità 2, 08034 Barcelona, Spain
5  Institut de Ciències de l'Espai (CSIC)

(Received 10 March 2004 / Accepted 16 July 2004)

We explore the adiabatic pulsational properties of massive white dwarf stars with hydrogen-rich envelopes and oxygen/neon and carbon/oxygen cores. To this end, we compute the cooling of massive white dwarf models for both core compositions taking into account the evolutionary history of the progenitor stars and the chemical evolution caused by time-dependent element diffusion. In particular, for the oxygen/neon models we adopt the chemical profile resulting from repeated carbon-burning shell flashes expected in very massive white dwarf progenitors. For carbon/oxygen white dwarfs we consider the chemical profiles resulting from phase separation upon crystallization. For both compositions we also take into account the effects of crystallization on the oscillation eigenmodes. We find that the pulsational properties of oxygen/neon white dwarfs are noticeably different from those made of carbon/oxygen, thus making asteroseismological techniques a promising way to distinguish between the two types of stars and, hence, to obtain valuable information about their progenitors.

Key words: stars: evolution -- stars: white dwarfs -- stars: oscillations

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© ESO 2004

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