2006A&A...458..259C


Query : 2006A&A...458..259C

2006A&A...458..259C - Astronomy and Astrophysics, volume 458, 259-267 (2006/10-4)

New nonadiabatic pulsation computations on full PG 1159 evolutionary models: the theoretical GW Virginis. instability strip revisited.

CORSICO A.H., ALTHAUS L.G. and MILLER BERTOLAMI M.M.

Abstract (from CDS):

We reexamine the theoretical instability domain of pulsating PG 1159 stars (GW Vir variables). We performed an extensive g-mode stability analysis on PG 1159 evolutionary models with stellar masses ranging from 0.530 to 0.741M, for which the complete evolutionary stages of their progenitors from the ZAMS, through the thermally pulsing AGB and born-again phases to the domain of the PG 1159 stars have been considered. We found that pulsations in PG 1159 stars are excited by the κ-mechanism due to partial ionization of carbon and oxygen, and that no composition gradients are needed between the surface layers and the driving region, much in agreement with previous studies. We show, for the first time, the existence of a red edge of the instability strip at high luminosities. We found that all of the GW Vir stars lay within our theoretical instability strip. Our results suggest a qualitative good agreement between the observed and the predicted ranges of unstable periods of individual stars. Finally, we found that generally the seismic masses (derived from the period spacing) of GW Vir stars are somewhat different from the masses suggested by evolutionary tracks coupled with spectroscopy. Improvements in the evolution during the thermally pulsing AGB phase and/or during the core helium burning stage and early AGB could help to alleviate the persisting discrepancies.

Abstract Copyright:

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

CDS comments: Fig.6 Some objects are not in Simbad (incomplete format).

Simbad objects: 22

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Number of rows : 22
N Identifier Otype ICRS (J2000)
RA
ICRS (J2000)
DEC
Mag U Mag B Mag V Mag R Mag I Sp type #ref
1850 - 2022
#notes
1 PB 5835 WD* 00 16 51.4153668936 -01 13 29.300107908   16 16.80 17.41   PG1159 17 0
2 NGC 246 PN 00 47 03.3420341616 -11 52 18.971126076 10.15 11.52 11.76 12.18   PG1159 466 0
3 PG 0122+200 WD* 01 25 22.5121704552 +20 17 56.963079924   16.2   16.9   DOZ.7 107 0
4 GD 1088 ** 01 32 39.347 -19 21 40.38   15.51 15.77 15.77   PG1159 45 0
5 M 76 PN 01 42 19.6557728208 +51 34 31.534970052     17.48   17.69 DOZ 366 2
6 NGC 1466 GlC 03 44 33 -71 40.3   11.6 11.59     ~ 160 0
7 KUV 03467-0108 WD* 03 49 17.4089215872 -00 59 19.230310320   18.0 17.81     PG1159 17 1
8 WRAY 17-1 PN 07 14 49.4240697984 -46 57 39.199063500   13.8 13.00     PG1159 78 0
9 PN A66 21 PN 07 29 02.7096654192 +13 14 48.587555184   15.67 15.99     DOZ 186 0
10 PN ARO 121 PN 07 57 51.6169237320 +53 25 16.950484848   16.775 17.128 17.288 17.501 DQ 158 1
11 PN Lo 4 PN 10 05 45.7880109408 -44 21 33.523482384           sdO 131 1
12 V* GW Vir WD* 12 01 45.9731868264 -03 45 40.628670300   14.87 15.04     DOQZ1 475 0
13 HE 1429-1209 WD* 14 32 20.7451392024 -12 22 48.253478808   15.7 16.15 16.27   PG1159 24 0
14 PG 1707+427 WD* 17 08 47.6869215528 +42 41 00.558430656   16.18       PG1159 112 0
15 PN A66 43 PN 17 53 32.2767758208 +10 37 24.210757560   14.53 14.71     O7fk 132 0
16 PN K 1-16 PN 18 21 52.1086837968 +64 21 53.406292104   14.44 14.96 15.26   PG1159 242 0
17 SH 2-68 PN 18 24 58.4294414904 +00 51 36.021249072   16.0 16.5     DAOZ.6 126 1
18 MWP 1 PN 21 17 08.2817782392 +34 12 27.415995372     12.33     PG1159 179 0
19 V* IR Peg WD* 21 34 08.2124719240 +06 50 57.662044329   16.15       PG1159 115 0
20 NGC 7094 PN 21 36 52.9687364088 +12 47 19.099274136     13.35     ~ 184 0
21 V* V409 And WD* 23 27 15.9353097240 +40 01 23.429781408   14.1 15.41     DO 73 0
22 PN Jn 1 PN 23 35 53.3214838680 +30 28 06.336745212   15.52 15.62     DOZ 102 0

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2022.05.28-00:26:32

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