The ZZ Ceti star G 185-32: new insight from asteroseismology

Details The ZZ Ceti star G 185-32: new insight from asteroseismology The ZZ Ceti star G 185-32: new insight from asteroseismology

Jul 2006

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2006a%26a...453..219p&link_type=abstract

Astronomy and Astrophysics, Volume 453, Issue 1, July I 2006, pp.219-227

Astronomy and Astrophysics

Astrophysics

6

Stars: Fundamental Parameters, Stars: White Dwarfs, Stars: Oscillations, Stars: Individul: Zz Ceti G 185-32

Scientific paper

One of the brightest pulsating DA white dwarfs (ZZ Ceti stars), G 185-32, shows 19 periods in its power spectrum, from 71 s to 651 s. Its short periods are among the shortest ones observed in a ZZ Ceti star. The one at 141.9 s shows an amplitude which does not vary with wavelength, in contrast with what the linear theory predicts for ℓ=1 or ℓ=2 non-radial g-modes. The mass and T_eff of G 185-32 are well constrained by spectroscopic observations and parallax measurement. The aim of the present paper is to take advantage of this rich observational background to derive the fundamental parameters of the star from asteroseismology. We computed a grid of realistic models for G 185-32 and the periods of their adiabatic ℓ=1 and ℓ=2 non-radial g-modes. We determined the model which fits best the observations. We identify 14 periods as real modes and determine their ℓ, k, and m values. We show that the remaining 5 periods are linear combinations.We find that G 185-32 oscillates mostly according to ℓ=2 modes. We present a new hypothesis to account for the peculiar behaviour of the 141.9 s mode's amplitude and suggest that it is a true mode interfering with higher ℓ degree modes, involving a possible triplet resonance. We determine the main parameters of G 185-32: its total mass M*=0.638 (±0.007) M&sun;, its hydrogen mass fraction M_H= 1.70 (±0.10) × 10-4 M*, which implies a helium mass fraction of ≈10-2 M{*}, its T_eff= 12 280 (±)80 K, and estimate its rotation period to be 14.5 h.

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