Journal
ASTRONOMY & ASTROPHYSICS
Volume 467, Issue 2, Pages L29-U7Publisher
EDP SCIENCES S A
DOI: 10.1051/0004-6361:20077250
Keywords
planetary nebulae : general; stars : evolution; stars : white dwarfs
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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 M-circle dot. Results. The CSPN mass distribution is sharply peaked at 0.61 M-circle dot. The WD distribution peaks at lower masses (0.58 M-circle dot) 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 Blocker 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.
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