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| Naji, M. |
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| Motta, Antonella |
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| Aletan, Dirar |
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| Mohamed, Tarek |
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| Ertürk, Emre |
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| Taccardi, Nicola |
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| Kononenko, Denys |
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| Petrov, R. H. | Madrid |
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| Alshaaer, Mazen | Brussels |
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| Bih, L. |
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| Casati, R. |
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| Muller, Hermance |
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| Kočí, Jan | Prague |
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| Šuljagić, Marija |
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| Kalteremidou, Kalliopi-Artemi | Brussels |
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| Azam, Siraj |
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| Ospanova, Alyiya |
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| Blanpain, Bart |
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| Ali, M. A. |
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| Popa, V. |
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| Rančić, M. |
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| Ollier, Nadège |
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| Azevedo, Nuno Monteiro |
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| Landes, Michael |
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| Rignanese, Gian-Marco |
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Werner, Klaus
University of Tübingen
in Cooperation with on an Cooperation-Score of 37%
Topics
Publications (9/9 displayed)
- 2019Spectral analysis of the hybrid PG 1159-type central stars of the planetary nebulae Abell 43 and NGC 7094citations
- 2018Metal abundances in hot white dwarfs with signatures of a superionized windcitations
- 2012Absorption Features in the Spectra of X-Ray Bursting Neutron Stars
- 2011What is the origin of the hottest known white dwarf?
- 2007Non-LTE modeling of supernova-fallback diskscitations
- 2007Abundances of Trace Elements in PG 1159 Stars
- 2007Soft X-ray Spectroscopy of the Hot DA White Dwarf LB 1919 and the PG 1159 Star PG 1520+525
- 2006Light Metals in PG1159 Central Stars
- 2005HST and FUSE Spectroscopy of Hot Hydrogen-Rich Central Stars of Planetary Nebulaecitations
Places of action
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document
Soft X-ray Spectroscopy of the Hot DA White Dwarf LB 1919 and the PG 1159 Star PG 1520+525
Abstract
We have performed soft X-ray spectroscopy of two hot white dwarfs with the Chandra observatory using the Low Energy Transmission Grating. The first target is the hot DA white dwarf LB 1919 (T<SUB>eff</SUB> = 69 000 K). This star is representative of a small group of hot DAs whose metallicities lie well below predictions from radiative levitation theory. The Chandra spectrum shows a rich absorption line spectrum which may allow to find the origin of the low-metallicity nature of these DAs. The second target is PG 1520+525, a very hot non-pulsating PG 1159 star. We find that it is hotter (T<SUB>eff</SUB> = 150 000 K) than the pulsating prototype PG 1159-035 (T<SUB>eff</SUB> = 140 000 K) and conclude that both stars confine the blue edge of the GW Vir instability strip....