| People | Locations | Statistics |
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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
HST and FUSE Spectroscopy of Hot Hydrogen-Rich Central Stars of Planetary Nebulae
Abstract
High-resolution UV spectra, obtained with HST and FUSE, enable us to analyse hot hydrogen-rich central stars in detail. Up to now, optical hydrogen and helium lines have been used to derive temperature and surface gravity. Those lines, however, are rather insensitive; in particular, neutral helium lines have completely vanished in the hottest central stars. Therefore, we have concentrated on ionization balances of metals, which have a rich line spectrum in the UV, to establish a new temperature scale for our sample. Furthermore, we have determined abundances of light metals, which had been poorly known before. They show considerable variation from star to star. We present results of quantitative spectral analyses performed with non-LTE model atmospheres....