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Far-Ultraviolet Temperature Diagnostics for Hot Central Stars of Planetary NebulaeThe effective temperature of hot central stars of planetary nebulae is usually determined from the ratios of optical He II lines. However, far-ultraviolet spectra from the FUSE satellite of several hot (T(sub eff) > 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, FeVII 1118.6, 1141.4, FeVI 1120.9, 1131.5, and NiVI 1124.2, 1148.2. The strong FVI 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 (T(sub eff)= 82000 K from He II vs 95000 K from Far-W metal lines) is presented.
Document ID
20090022376
Acquisition Source
Goddard Space Flight Center
Document Type
Conference Paper
Authors
Sonneborn, G.
(NASA Goddard Space Flight Center Greenbelt, MD, United States)
Ipin, R. C.
(NASA Goddard Space Flight Center Greenbelt, MD, United States)
Herald, J.
(Johns Hopkins Univ. MD, United States)
Date Acquired
August 24, 2013
Publication Date
January 7, 2007
Subject Category
Astrophysics
Meeting Information
Meeting: American Astronoical Society Meeting
Location: Seattle, WA
Country: United States
Start Date: January 7, 2007
End Date: January 10, 2007
Distribution Limits
Public
Copyright
Other

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