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Preprint 10/10

Metal abundances in the hottest known DO white dwarf (KPD0005+5106)

D. Wassermann (1), K. Werner (1), T. Rauch (1), J.W. Kruk (2)

(1) Institute for Astronomy and Astrophysics, Kepler Center for Astro and Particle Physics, Eberhard Karls Universität Tübingen, Sand 1, 72076 Tübingen, Germany
(2) Department of Physics and Astronomy, Johns Hopkins University, Baltimore, MD 21218, USA; current address: NASA Goddard Space Flight Center, Greenbelt, MD 20771, USA

To be published in: A&A

Abstract. We present the analysis of ultraviolet and optical spectra of KPD0005+5106. Redetermination of the atmospheric parameters is necessary because the recent discovery of highly ionised metals (NeVIII, CaX) indicates that the effective temperature is significantly higher than previously thought. Here we announce the discovery of lines from highly ionised silicon, sulphur, and iron (SiVII, SVII, FeX) which were never found before in any stellar photosphere. Our analysis of these lines and those from helium and several other metals gives T_eff = 200,000 ± 20,000 K, log g = 6.7 ± 0.3. Mass and luminosity follow from a comparison with evolutionary tracks: M = 0.64M_sun and log L/L_sun = 3.7, so that, strictly speaking, the star is a helium-burning pre-white dwarf. The mass fractions of the metals in the helium-dominated atmosphere are in the range 0.7-4.3 solar. Hydrogen is not detectable and we derive an upper abundance limit of 0.034 solar. This abundance pattern is probably unaffected by gravitational settling and radiative levitation. Its origin lies in previous evolutionary stages. We discuss the link of KPD0005+5106 to RCrB stars and the possibility that it results from a double-degenerate merger event.
 

Preprint (476 kb PDF file including figures)

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