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New models for the evolution of central stars of planetary nebulae: Faster and Brighter

Published online by Cambridge University Press:  08 August 2017

Marcelo M. Miller Bertolami
Marcelo M. Miller Bertolami*
Affiliation:
Instituto de Astrofisica de La Plata, CONICET-UNLP, Paseo del Bosque s/n, (B1900FWA) La Plata, Argentina. email: mmiller@fcaglp.unlp.edu.ar
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Abstract

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The post-asymptotic giant branch (AGB) phase is arguably one of the least understood phases of the evolution of low- and intermediate- mass stars. The recent post-AGB evolutionary sequences computed by Miller Bertolami (2016) are at least three to ten times faster than those previously published by Vassiliadis & Wood (1994) and Blöcker (1995) which have been used in a large number of studies. This is true for the whole mass and metallicity range. The new models are also ~0.1–0.3 dex brighter than the previous models with similar remnant masses. In this short article we comment on the main reasons behind these differences, and discuss possible implications for other studies of post-AGB stars or planetary nebulae.

Keywords

stars: AGB and post-AGBplanetary nebulae: general
Type
Contributed Papers
Information
Proceedings of the International Astronomical Union , Volume 12 , Symposium S323: Planetary Nebulae: Multi-Wavelength Probes of Stellar and Galactic Evolution , October 2016 , pp. 179 - 183
Copyright
Copyright © International Astronomical Union 2017 

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