Astronomy and Astrophysics – Astronomy
Scientific paper
Dec 2006
adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2006aas...209.9203s&link_type=abstract
2007 AAS/AAPT Joint Meeting, American Astronomical Society Meeting 209, #92.03; Bulletin of the American Astronomical Society, V
Astronomy and Astrophysics
Astronomy
Scientific paper
The effective temperatures of central stars of planetary nebulae are usually determined from the ratios of optical He II lines. However, far-ultraviolet spectra from the FUSE satellite of several hot (Teff > 70,000 K) hydrogen-rich central stars have stellar features that imply a significantly hotter effective temperature than that determined from He II. There are many stellar features in the long wavelength portion of the FUSE spectrum. These include O VI 1146-47, F VI 1039.5, Fe VII 1118.6, 1141.4, Fe VI 1120.9, 1131.5, and Ni VI 1124.2, 1148.2. The strong F VI 1139.5 line is of interest because of the large overabundance (over 100X solar) of F in some PG1159 stars reported recently by Werner et al. (2005). Modeling these spectral features may provide an method for measuring the effective temperature of these stars independent of the He II lines. An example of HD 200516, the central star of NGC 7009 (Teff = 82000 K from He II vs 95000 K from Far-UV metal lines) is presented. The FUSE observations were obtained under GI program C176. This work has been supported in part by NASA grant NAG5-12347 to Catholic University of America.
Herald James
Iping Rosina
Sonneborn George
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