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The Stellar Wind From the Central Star of NGC 7009

Published online by Cambridge University Press:  15 December 2006

G. Sonneborn
Affiliation:
Lab. for Observational Cosmology, Code 665, NASA/GSFC, Greenbelt, MD 20771 USA email: george.sonneborn@nasa.gov
R. C. Iping
Affiliation:
Lab. for Observational Cosmology, Code 665, NASA/GSFC, Greenbelt, MD 20771 USA email: george.sonneborn@nasa.gov Dept. of Physics, Catholic University of America, Washington, DC 20064 USA
D. L. Massa
Affiliation:
Lab. for Observational Cosmology, Code 665, NASA/GSFC, Greenbelt, MD 20771 USA email: george.sonneborn@nasa.gov SGT, Inc., Greenbelt, MD 20770 USA
Y-H Chu
Affiliation:
Dept. of Astronomy, University of Illinois, Urbana, IL 61801 USA
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Abstract

High-resolution 905-1187Å spectra of the central star of NGC 7009 obtained with the FUSE satellite provide new constraints on the mass loss and atmosphere parameters. The most prominent spectral feature is a very strong P-Cygni profile of O VI 1032-1038. The only other wind lines are S VI 933-44 (FUSE) and N V 1238-42 and O V 1371 from IUE spectra. C IV 1548-50 and P V 1118-28 are not present, indicating that the wind is very highly ionized. A lower limit on the mass loss rate ($\dot{M}>10^{-8} M_{\odot} $y$^{-1}, v_{\infty}=2450$ km s$^{-1}$) has been derived from an SEI analysis of these wind lines. Preliminary identification of several photospheric spectral features include several strong Fe VII and O VI lines between 1100 and 1170 Å.

Type
Contributed Papers
Copyright
© 2006 International Astronomical Union

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