Volume 467, Number 2, May IV 2007
|Page(s)||L29 - L32|
|Published online||11 April 2007|
Letter to the Editor
White dwarf masses derived from planetary nebula modelling*
Centrum Astronomii UMK, ul. Gagarina 11, 87-100 Torun, Poland e-mail: Krzysztof.Gesicki@astri.uni.torun.pl
2 School of Physics and Astronomy, University of Manchester, PO Box 88, Manchester M60 1QD, UK e-mail: email@example.com
Accepted: 15 March 2007
Aims.We compare the mass distribution of central stars of planetary nebulae (CSPNe) with those of their progeny, white dwarfs (WD).
Methods.We use a dynamical method to measure masses with an uncertainty of 0.02 .
Results.The CSPN mass distribution is sharply peaked at . The WD distribution peaks at lower masses () and shows a much broader range of masses. Some of the difference can be explained if the early post-AGB evolution is faster than predicted by the Blöcker tracks. Between 30 and 50 per cent of WD may avoid the PN phase because they have too low a mass. However, the discrepancy cannot be fully resolved and WD mass distributions may have been broadened by observational or model uncertainties.
Key words: planetary nebulae: general / stars: evolution / stars: white dwarfs
© ESO, 2007
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