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Spectral analysis of the O(He)-type central stars of the planetary nebulae K 1-27 and LoTr 4

Published online by Cambridge University Press:  30 August 2012

Nicole Reindl
Affiliation:
Institute for Astronomy and Astrophysics, Kepler Center for Astro and Particle Physics, Eberhard Karls University, Sand 1, 72076 Tübingen, Germany email: reindl@astro.uni-tuebingen.de
Ellen Ringat
Affiliation:
Institute for Astronomy and Astrophysics, Kepler Center for Astro and Particle Physics, Eberhard Karls University, Sand 1, 72076 Tübingen, Germany email: reindl@astro.uni-tuebingen.de
Thomas Rauch
Affiliation:
Institute for Astronomy and Astrophysics, Kepler Center for Astro and Particle Physics, Eberhard Karls University, Sand 1, 72076 Tübingen, Germany email: reindl@astro.uni-tuebingen.de
Klaus Werner
Affiliation:
Institute for Astronomy and Astrophysics, Kepler Center for Astro and Particle Physics, Eberhard Karls University, Sand 1, 72076 Tübingen, Germany email: reindl@astro.uni-tuebingen.de
Jeffrey. W. Kruk
Affiliation:
NASA Goddard Space Flight Center, Greenbelt, MD 20771, U.S.A.
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Abstract

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The four known O(He) stars are the only amongst the hottest post-AGB stars whose atmospheres are composed of almost pure helium. Thus, their evolution deviates from the hydrogen-deficient post-AGB evolutionary sequence of carbon-dominated stars like e.g. PG 1159 stars. The origin of the O(He) stars is still not explained. They might be either post-early AGB stars or the progeny of R Coronae Borealis stars. We present preliminary results of a non-LTE spectral analysis based on FUSE and HST/COS observations.

Type
Contributed Papers
Copyright
Copyright © International Astronomical Union 2012

References

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