Computer Science
Scientific paper
May 2009
adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2009aipc.1135..171r&link_type=abstract
FUTURE DIRECTIONS IN ULTRAVIOLET SPECTROSCOPY: A Conference Inspired by the Accomplishments of the Far Ultraviolet Spectroscopic
Computer Science
1
Stellar Clusters And Associations, Faint Blue Stars, White Dwarfs, Degenerate Stars, Nuclei Of Planetary Nebulae, Photochemistry
Scientific paper
State-of-the-art non-LTE spectral analysis requires high-resolution and high-S/N observations of strategic metal lines in order to achieve reliable photospheric parameters like, e.g., effective temperature, surface gravity, and element abundances.
Hot stars with effective temperatures higher than about 40 000 K exhibit their metal-line spectrum arising from highly ionized species predominantly in the (far) ultraviolet wavelength range.
FUSE observations of hot, compact stars provided the necessary data. With these, it has been, e.g., possible to identify fluorine for the first time in observations of post-AGB stars. The evaluation of ionization equilibria of highly ionized neon, phosphorus, sulfur, and argon provides a new sensitive tool to determine effective temperatures of the hottest stars precisely. Moreover, abundance determinations have put constraints on stellar evolutionary models which, in turn, have improved greatly our picture of post-AGB evolution.
Koesterke Lars
Kruk Jeff W.
Oliveira Cristina M.
Rauch Thomas
Werner Kirstin
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