Query : 2009A&A...506..835C

2009A&A...506..835C - Astronomy and Astrophysics, volume 506, 835-843 (2009/11-1)

Hot C-rich white dwarfs: testing the DB-DQ transition through pulsations.


Abstract (from CDS):

Hot DQ white dwarfs are a new class of white dwarf stars that were discovered recently within the framework of the SDSS project. There are nine known hot DQ stars, out of a total of several thousands white dwarfs spectroscopically identified. Three hot DQ white dwarfs have been reported to exhibit photometric variability with periods compatible with pulsation g-modes. We present a nonadiabatic pulsation analysis of carbon-rich hot DQ white dwarf stars. One of our main aims is to test the convective-mixing scenario for the origin of hot DQs by studying their pulsational properties. Our pulsation study is based on the full evolutionary models of hot DQ white dwarfs developed by Althaus and collaborators, which consistently cover the entire evolution from the born-again stage to the white dwarf cooling track. Specifically, we present a stability analysis of white dwarf models from stages before the blue edge of the DBV instability strip (Teff≃30000K), until the domain of the hot DQ white dwarfs (18000-24000K), including the transition DB->hot DQ white dwarf. We explore evolutionary models with M*=0.585M and M*=0.87M, and two values of the thickness of the He-rich envelope (MHe=2x10–7M* and MHe=10–8M*). These envelopes are 4-5 orders of magnitude thinner than those of standard DB white dwarf models resulting from canonical stellar evolution computations. We found that at evolutionary phases in which the models are characterized by He-dominated atmospheres, they exhibit unstable g-mode pulsations typical of DBV stars, and when the models become DQ white dwarfs with carbon-dominated atmospheres, they continue being pulsationally unstable with characteristics similar to DB models, and in agreement with the periods detected in variable hot DQ white dwarfs. In particular, for models with MHe=10–8M*, a narrow gap exists separating the DB from the DQ instability domains. Our calculations provide strong support for the convective-mixing picture of the formation of hot DQs. In particular, our results suggest the existence of pulsating DB white dwarfs with very thin He-rich envelopes, which after passing the DBV instability strip become variable hot DQ stars. The existence of these DB stars with very thin envelopes should be investigated by asteroseismology.

Abstract Copyright:

Journal keyword(s): stars: evolution - stars: interiors - stars: oscillations - white dwarfs

Simbad objects: 7

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Number of rows : 7
N Identifier Otype ICRS (J2000)
ICRS (J2000)
Mag U Mag B Mag V Mag R Mag I Sp type #ref
1850 - 2024
1 V* SW LMi WD* 09 57 49.4086247376 +33 59 23.691674976   17       DB 56 0
2 GALEX J142625.6+575218 WD* 14 26 25.7057882376 +57 52 18.263585532   19.7 19.37 19.5   DQ 29 1
3 PG 1501+664 WD* 15 02 09.6299323152 +66 12 19.148868324   16.07 16.37     DZQ1 156 0
4 GD 358 WD* 16 47 18.3925183824 +32 28 32.862804384 12.511 13.530 13.653 13.752 13.852 DB2 348 0
5 V* QU Tel WD* 20 09 40.1871967824 -52 25 15.864452508 14.51 15.25 15.03     DB2 54 1
6 PB 7043 WD* 22 00 29.0935424040 -07 41 21.646986144   18       DQ 24 0
7 PB 7970 WD* 23 48 43.3128871272 -09 42 45.345807252   19       DQ 21 0

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