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A&A 467, L29-L32 (2007)
DOI: 10.1051/0004-6361:20077250
Letter
White dwarf masses derived from planetary nebula modelling
K. Gesicki1 and A. A. Zijlstra21 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: a.zijlstra@manchester.ac.uk
(Received 7 February 2007 / Accepted 15 March 2007)
Abstract
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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