White dwarf masses derived from planetary nebulae modelling

Details White dwarf masses derived from planetary nebulae modelling White dwarf masses derived from planetary nebulae modelling

2007-04-04

arxiv.org/abs/0704.0620v1

Astronomy and Astrophysics

Astrophysics

4 pages, accepted for A&A Letters

Scientific paper

10.1051/0004-6361:20077250

We compare the mass distribution of central stars of planetary nebulae (CSPN) with those of their progeny, white dwarfs (WD). We use a dynamical method to measure masses with an uncertainty of 0.02 M$_\odot$. The CSPN mass distribution is sharply peaked at $0.61 \rm M_\odot$. The WD distribution peaks at lower masses ($0.58 \rm M_\odot$) 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 Bl\"ocker tracks. Between 30 and 50 per cent of WD may avoid the PN phase because of too low 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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