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The Effects of Transition Time on the Populations of Post-AGB Stars, and on the Nebular Evolution

Published online by Cambridge University Press:  26 May 2016

Eva Villaver
Affiliation:
Space Telescope Science Instituto, 3700 San Martin Drive, Baltimore, MD 21218, USA
Letizia Stanghellini
Affiliation:
Space Telescope Science Instituto, 3700 San Martin Drive, Baltimore, MD 21218, USA
Arturo Manchado
Affiliation:
Institute de Astrofísica de Canarias, c/ Via Láctea s/n 38200 La Laguna (Tenerife), Spain
Guillermo García-Segura
Affiliation:
Instituto de Astronomía-Universidad Nacional Autónoma de México, Apartado Postal 877, Ensenada, 22830 Baja California, México
Alvio Renzini
Affiliation:
European Southern Observatory, Karl-Schwarzschild-Str. 2, 85748 Garching, Germany

Abstract

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We show how the different assumptions on the transition time (the time lag between the superwind quenching at the AGB and the illumination of the Planetary Nebula [PN]) reflect into very different theoretical outcomes, both in the characteristics of the stellar remnants, and in the evolution of the nebular shells.

We use a Monte Carlo simulation of post-AGB stars with a set of assumptions on the transition time, to show the effect on the resulting location of the stars on the HR diagram, and on the derived core mass distributions.

We have also performed numerical simulations of the PN formation process, and investigated the effects of the transition time on the resulting PN structure. We found that the transition time determines not only the size of the PN shell, but also its dynamical evolution.

We show the important implications that the transition time has on the observable parameters during the PN stage.

Type
Part III: Planetary Nebulae in the Scheme of Stellar Evolution
Copyright
Copyright © Astronomical Society of the Pacific 2003 

References

Stanghellini, L. & Renzini, A. 2000, ApJ, 542, 308 CrossRefGoogle Scholar
Vassiliadis, E. & Wood, P. 1994, ApJS, 92, 125 CrossRefGoogle Scholar
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