Abstract
We review our current knowledge about hot helium rich (DO) white dwarfs. For most known DOs detailed NLTE model atmosphere analysis have now become available. These stars represent the non-DA white dwarf cooling sequence from the hot end (T eff≈120 000 K) down to the DB gap (T eff ≈45 000 K). Determination of effective temperature, surface gravity and metallicities allow a comprehensive comparison with predictions of diffusion calculations.
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Dreizler, S., Werner, K. (1997). Non-LTE Analyses of DO White Dwarfs. In: Isern, J., Hernanz, M., García-Berro, E. (eds) White Dwarfs. Astrophysics and Space Science Library, vol 214. Springer, Dordrecht. https://doi.org/10.1007/978-94-011-5542-7_30
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DOI: https://doi.org/10.1007/978-94-011-5542-7_30
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