Temperature scale and metal abundances of hot hydrogen-rich central stars of planetary nebulae

Details Temperature scale and metal abundances of hot hydrogen-rich central stars of planetary nebulae Temperature scale and metal abundances of hot hydrogen-rich central stars of planetary nebulae

Jul 2000

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2000hst..prop.8638w&link_type=abstract

HST Proposal ID #8638

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Hst Proposal Id #8638 Hot Stars

Scientific paper

We propose UV spectroscopy of a sample of hot hydrogen-rich central stars of PNe, covering the hottest phase of post-AGB evolution {T_eff > 70 000 K}. The spectra shall be analyzed with fully metal line blanketed NLTE model atmospheres in order to determine T_eff, surface gravity, and chemical composition. The results will address the following problems: 1. The temperature scale of the hottest central stars is poorly known. Iron lines, only accessible in the UV, are ideal temperature indicators to set up a reliable temperature scale. 2. Depending on the particular star, the derived metal abundances are either dominated by current diffusion processes or they originate from dredge-up phases during previous AGB evolution. We expect that our sample comprises different objects so that both processes/phases can be studied in detail. 2a. Those objects, which show qualitatively a metal abundance pattern which points at dredge-up phases, can be used to quantitatively check against abundance predictions of stellar evolution theory. 2b. The other objects, where gravitational diffusion and radiative acceleration determine the photospheric metal abundances, will be used to check our NLTE models which for the first time include diffusion processes self-consistently.

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