Volume 441, Number 1, October I 2005
|Page(s)||231 - 233|
|Section||Stellar structure and evolution|
|Published online||13 September 2005|
The nature of the driving mechanism in the pulsating hybrid PG 1159 star Abell 43
Département de Physique, Université de Montréal, CP 6128, Succ. Centre-Ville, Montréal, Québec H3C 3J7, Canada e-mail: [quirion;fontaine;brassard]@astro.umontreal.ca
Accepted: 23 May 2005
We extend our previous pulsational stability analyses of PG 1159 stars by modeling the hybrid PG 1159 type star Abell 43. We show that the standard κ-mechanism due to the ionization of C and O in the envelope of this H-rich PG 1159 star is perfectly able to drive g-mode pulsations. Thus, contrary to a recent suggestion, there is no need to invoke any new or exotic mechanism to explain the pulsational instabilities observed in this particular star. Our expected instability band for modes extends in period from ~2604 s to ~5529 s, which is consistent with the available photometric observations of Abell 43. We also suggest that efforts to detect luminosity variations in its sibling NGC 7094 be pursued.
Key words: stars: white dwarfs / stars: oscillations / stars: individual: Abell 43
© ESO, 2005
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