Talk abstract details
(F)UV Spectroscopy of 15 Extremely Hot Central Stars of Planetary Nebulae
Abstract
We present results of (F)UV spectral analyses of 15 CSPNe of DAO-type (A\,7, A\,31, A\,35, A\,39, NGC\,3587, NGC\,6720, NGC\,6853, NGC\,7293, PuWe\,1, Sh\,$2-174$) and O(H)-type (A\,36, Lo\,1, LSS\,1362, NGC\,1360, NGC\,4361) CSPNe, based on NLTE model atmospheres.
We aim especially at a precise determination of $T_\mathrm{eff}$ by evaluation of ionization equilibria of many species and ionization stages. This is the prerequisite for $\log g$ and abundance determinations. The derived parameters are crucial constraints for predictions of AGB nucleosynthesis as well as stellar evolution calculations.
Additional modeling of the ISM line-absorption enables to unambigiously identify nearly all observed lines and to improve both, the photospheric as well as the ISM model.
We aim especially at a precise determination of $T_\mathrm{eff}$ by evaluation of ionization equilibria of many species and ionization stages. This is the prerequisite for $\log g$ and abundance determinations. The derived parameters are crucial constraints for predictions of AGB nucleosynthesis as well as stellar evolution calculations.
Additional modeling of the ISM line-absorption enables to unambigiously identify nearly all observed lines and to improve both, the photospheric as well as the ISM model.