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S-process Elements in Binary Central Stars of Planetary Nebulae

Published online by Cambridge University Press:  30 December 2019

Lisa Löbling Open the ORCID record for Lisa Löbling [Opens in a new window]  and
Henri Boffin
Lisa Löbling
Affiliation:
European Southern Observatory, Karl-Schwarzschild-Str. 2, 85748 Garching bei München, Germany email: lloebling@eso.org Institute for Astronomy and Astrophysics, Kepler Center for Astro and Particle Physics, Eberhard Karls University, Sand 1, 72076 Tübingen, Germany
Henri Boffin
Affiliation:
European Southern Observatory, Karl-Schwarzschild-Str. 2, 85748 Garching bei München, Germany email: lloebling@eso.org
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Abstract

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Low- and intermediate-mass stars experience a phase of carbon enrichment and slow neutron-capture nucleosynthesis (s-process) on the asymptotic giant branch. An interesting element is the radioactive technetium, whose presence is a clear indication that nucleosynthesis happened recently. Analysing the element abundances not only in the hot evolved stars at the center of planetary nebulae helps to derive constraints for the evolution of these stars. Doing so also in their companions if they are in a binary, provides information on the mass-transfer history.

Keywords

planetary nebulae: individual: Hen 2–39stars: abundancesstars: evolutionAGB and post-AGB starschemically peculiar stars: barium-stars
Type
Contributed Papers
Information
Proceedings of the International Astronomical Union , Volume 14 , Symposium S343: Why Galaxies Care About AGB Stars: A Continuing Challenge through Cosmic Time , August 2018 , pp. 452 - 453
Copyright
© International Astronomical Union 2019 

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