2007A&A...462..281J


C.D.S. - SIMBAD4 rel 1.7 - 2019.08.19CEST04:28:57

2007A&A...462..281J - Astronomy and Astrophysics, volume 462, 281-292 (2007/1-4)

High-resolution ultraviolet spectroscopy of PG 1159-035 with HST and FUSE.

JAHN D., RAUCH T., REIFF E., WERNER K., KRUK J.W. and HERWIG F.

Abstract (from CDS):

PG 1159-035 is the prototype of the PG 1159 spectral class which consists of extremely hot hydrogen-deficient (pre-) white dwarfs. It is also the prototype of the GW Vir variables, which are non-radial g-mode pulsators. The study of PG 1159 stars reveals insight into stellar evolution and nucleosynthesis during AGB and post-AGB phases. We perform a quantitative spectral analysis of PG 1159-035 focusing on the abundance determination of trace elements. We have taken high-resolution ultraviolet spectra of PG 1159-035 with the Hubble Space Telescope and the Far Ultraviolet Spectroscopic Explorer. They are analysed with non-LTE line blanketed model atmospheres. We confirm the high effective temperature with high precision (Teff=140000±5000K) and the surface gravity of logg=7. For the first time we assess the abundances of silicon, phosphorus, sulfur, and iron. Silicon is about solar. For phosphorus we find an upper limit of solar abundance. A surprisingly strong depletion of sulfur (2% solar) is discovered. Iron is not detected, suggesting an upper limit of 30% solar. This coincides with the Fe deficiency found in other PG 1159 stars. We redetermine the nitrogen abundance and find it to be lower by one dex compared to previous analyses. The sulfur depletion is in contradiction with current models of AGB star intershell nucleosynthesis. The iron deficiency confirms similar results for other PG 1159 stars and is explained by the conversion of iron into heavier elements by n-capture in the s-processing environment of the precursor AGB star. However, the extent of the iron depletion is stronger than predicted by evolutionary models. The relatively low nitrogen abundance compared to other pulsating PG 1159 stars weakens the role of nitrogen as a distinctive feature of pulsators and non-pulsators in the GW Vir instability strip.

Abstract Copyright:

Journal keyword(s): stars: abundances - stars: atmospheres - stars: evolution - stars: individual: PG 1159-035 - stars: AGB and post-AGB

Simbad objects: 9

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Number of rows : 9

N Identifier Otype ICRS (J2000)
RA
ICRS (J2000)
DEC
Mag U Mag B Mag V Mag R Mag I Sp type #ref
1850 - 2019
#notes
1 NGC 246 PN 00 47 03.3420803259 -11 52 18.975106178 10.15 11.52 11.76 12.18   PG1159 448 0
2 PN Lo 4 PN 10 05 45.7878014012 -44 21 33.523563573           sdO 124 1
3 PG 1144+005 WD* 11 46 35.2287794057 +00 12 33.539708785   14.59 14.9     PG1159 78 0
4 V* GW Vir WD* 12 01 45.9728868858 -03 45 40.627851273   14.87 15.04     DOQZ1 456 0
5 PG 1707+427 WD* 17 08 47.6869967260 +42 41 00.558830272   16.18       PG1159 105 0
6 V* V4334 Sgr NL* 17 52 32.69 -17 41 08.0   12.01       F2Ia 318 0
7 PN K 1-16 PN 18 21 52.1081781582 +64 21 53.413814961   14.44 14.96 15.26   PG1159 228 0
8 MWP 1 PN 21 17 08.2817539788 +34 12 27.415871206     12.33     PG1159 172 0
9 NGC 7094 PN 21 36 52.9688055651 +12 47 19.100520826     13.35     ~ 173 0

    Equat.    Gal    SGal    Ecl

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2019.08.19-04:28:57

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