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(F)UV spectral analysis of 15 extremely hot, hydrogen-rich central stars of planetary nebulae

Published online by Cambridge University Press:  30 August 2012

Marc Ziegler
Affiliation:
Institute for Astronomy and Astrophysics, Kepler Center for Astro and Particle Physics, Eberhard Karls University, Tübingen, Germany email: ziegler@astro.uni-tuebingen.de
Thomas Rauch
Affiliation:
Institute for Astronomy and Astrophysics, Kepler Center for Astro and Particle Physics, Eberhard Karls University, Tübingen, Germany email: ziegler@astro.uni-tuebingen.de
Klaus Werner
Affiliation:
Institute for Astronomy and Astrophysics, Kepler Center for Astro and Particle Physics, Eberhard Karls University, Tübingen, Germany email: ziegler@astro.uni-tuebingen.de
Jeffrey W. Kruk
Affiliation:
NASA Goddard Space Flight Center, Greenbelt, U.S.A.
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Abstract

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We present results of a (F)UV spectral analysis of 15 hot, hydrogen-rich central stars of planetary nebulae (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). The sample covers a wide range of parameters (Teff ≈ 70–130 kK, log g = 5.4–7.4). It represents different stages of post-AGB evolution. The derived stellar parameters are crucial constraints for AGB nucleosynthesis and stellar evolutionary calculations. Detailed spectral analyses using fully line-blanketed NLTE model atmospheres including 23 elements from hydrogen to nickel are performed. 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.

Type
Contributed Papers
Copyright
Copyright © International Astronomical Union 2012

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