2018A&A...613A..46D


C.D.S. - SIMBAD4 rel 1.7 - 2021.04.11CEST14:13:44

2018A&A...613A..46D - Astronomy and Astrophysics, volume 613A, 46-46 (2018/5-1)

Asteroseismology of ZZ Ceti stars with full evolutionary white dwarf models. II. The impact of AGB thermal pulses on the asteroseismic inferences of ZZ Ceti stars.

DE GERONIMO F.C., ALTHAUS L.G., CORSICO A.H., ROMERO A.D. and KEPLER S.O.

Abstract (from CDS):

Context. The thermally pulsing phase on the asymptotic giant branch (TP-AGB) is the last nuclear burning phase experienced by most low- and intermediate-mass stars. During this phase, the outer chemical stratification above the C/O core of the emerging white dwarf (WD) is built up. The chemical structure resulting from progenitor evolution strongly impacts the whole pulsation spectrum exhibited by ZZ Ceti stars, which are pulsating C/O core white dwarfs located on a narrow instability strip at Teff∼12000K. Several physical processes occurring during progenitor evolution strongly affect the chemical structure of these stars; those found during the TP-AGB phase are the most relevant for the pulsational properties of ZZ Ceti stars. Aims. We present a study of the impact of the chemical structure built up during the TP-AGB evolution on the stellar parameters inferred from asteroseismological fits of ZZ Ceti stars. Methods. Our analysis is based on a set of carbon-oxygen core white dwarf models with masses from 0.534 to 0.6463M derived from full evolutionary computations from the ZAMS to the ZZ Ceti domain. We computed evolutionary sequences that experience different number of thermal pulses (TP). Results. We find that the occurrence or not of thermal pulses during AGB evolution implies an average deviation in the asteroseimological effective temperature of ZZ Ceti stars of at most 8% and on the order of ≤5% in the stellar mass. For the mass of the hydrogen envelope, however, we find deviations up to 2 orders of magnitude in the case of cool ZZ Ceti stars. Hot and intermediate temperature ZZ Ceti stars show no differences in the hydrogen envelope mass in most cases. Conclusions. Our results show that, in general, the impact of the occurrence or not of thermal pulses in the progenitor stars is not negligible and must be taken into account in asteroseismological studies of ZZ Ceti stars.

Abstract Copyright: © ESO 2018

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

Simbad objects: 14

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Number of rows : 14

N Identifier Otype ICRS (J2000)
RA
ICRS (J2000)
DEC
Mag U Mag B Mag V Mag R Mag I Sp type #ref
1850 - 2021
#notes
1 JL 197 WD* 00 33 36.1025997744 -55 08 38.947225117   15.89 15.73 15.90   DA 17 0
2 GD 1400 WD* 01 47 21.8246239967 -21 56 51.387203270   15.38 15.15 15.42   DA4.1 71 0
3 PB 9102 WD* 02 14 06.7838431307 -08 23 18.435727676   18.5       DA 16 0
4 V* VY Hor WD* 03 43 29.0337379468 -45 49 04.233992041   15.16 14.91 15.28   DA4.3 58 0
5 HL Tau 76 WD* 04 18 56.6380318051 +27 17 48.312463115   15.40       DA4.3 131 0
6 V* BR Cam WD* 04 59 27.2436978084 +55 25 21.054241072   15.98   16.1   DA4.3 60 0
7 NGC 2808 GlC 09 12 03.10 -64 51 48.6   7.77 5.69     ~ 1285 0
8 V* RY LMi WD* 09 24 15.2484202569 +35 16 51.400826911   15.72   15.99   DA4 252 0
9 SDSS J100238.56+581835.9 WD* 10 02 38.5728540973 +58 18 36.008035352   17.8   18.5   DA 12 0
10 V* IZ UMa WD* 11 39 41.4109194194 +42 05 18.427748207     16.56     DA4.1 33 0
11 HE 1429-0343 WD* 14 32 03.2156295169 -03 56 38.032926957   16.1 15.8 16.0   DA4.3 13 0
12 SDSS J150207.02-000147.1 WD* 15 02 07.0180632310 -00 01 47.243338657           DA3.5 17 0
13 EGGR 450 WD* 21 49 59.1885701911 +54 08 39.498906572   16.2   16.1   DA4.2 23 0
14 V* HW Aqr WD* 23 51 22.0903868280 -24 08 17.326639274   15.52   15.1   DA4.2 36 0

    Equat.    Gal    SGal    Ecl

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