(F)UV Spectral Analysis of Hot, Hydrogen-Rich Central Stars of Planetary Nebulae

Details (F)UV Spectral Analysis of Hot, Hydrogen-Rich Central Stars of Planetary Nebulae (F)UV Spectral Analysis of Hot, Hydrogen-Rich Central Stars of Planetary Nebulae

Nov 2010

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2010aipc.1273..235z&link_type=abstract

17TH EUROPEAN WHITE DWARF WORKSHOP. AIP Conference Proceedings, Volume 1273, pp. 235-238 (2010).

Physics

Planetary Nebulae, Spectral Analysis, Nucleosynthesis, Interstellar Matter, Photosphere, Planetary Nebulae, Luminosities, Magnitudes, Effective Temperatures, Colors, And Spectral Classification, Stellar Structure, Interiors, Evolution, Nucleosynthesis, Ages, Physical Properties, Stellar Atmospheres, Radiative Transfer, Opacity And Line Formation

Scientific paper

Metal abundances of CSPNe are not well known although they provide important constraints on AGB nucleosynthesis. We aim to determine metal abundances of two hot, hydrogen-rich CSPNe (namely of A35 and NGC3587, the latter also known as M97 or the Owl Nebula) and to derive Teff and log g precisely from high-resolution, high-S/N (far-) ultraviolet observations obtained with FUSE and HST/STIS. For this purpose, we utilize NLTE model atmospheres calculated with TMAP, the Tübingen Model Atmosphere Package. Due to strong line absorption of the ISM, simultaneous modeling of interstellar features has become a standard tool in our analyses. We present preliminary results, demonstrating the importance of combining stellar and interstellar models, in order to clearly identify and measure the strengths of strategic photospheric lines.

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