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Abundances of s-process elements in planetary nebulae: Br, Kr & Xe

Published online by Cambridge University Press:  15 December 2006

Y. Zhang ,
R. Williams ,
E. Pellegrini ,
K. Cavagnolo ,
J. A. Baldwin ,
B. Sharpee ,
M. Phillips  and
X.-W. Liu
Y. Zhang
Affiliation:
Department of Astronomy, Peking University, Beijing 100871, P. R. China Space Telescope Science Institute, 3700 San Martin Drive, Baltimore, MD 21218, USA
R. Williams
Affiliation:
Space Telescope Science Institute, 3700 San Martin Drive, Baltimore, MD 21218, USA
E. Pellegrini
Affiliation:
Department of Physics & Astronomy, Michigan State University, East Lansing, MI 48824, USA
K. Cavagnolo
Affiliation:
Department of Physics & Astronomy, Michigan State University, East Lansing, MI 48824, USA
J. A. Baldwin
Affiliation:
Department of Physics & Astronomy, Michigan State University, East Lansing, MI 48824, USA
B. Sharpee
Affiliation:
SRI International, 333 Ravenswood Ave. Menlo Park, CA 94025, USA
M. Phillips
Affiliation:
Las Campanas Observatory, Carnegie Observatories, Casilla 601, La Serena, Chile
X.-W. Liu
Affiliation:
Department of Astronomy, Peking University, Beijing 100871, P. R. China
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Abstract

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We identify emission lines of post-iron peak elements in very high signal-to-noise spectra of a sample of planetary nebulae. Analysis of lines from ions of Kr and Xe reveals enhancements in most of the PNe, in agreement with theories of $s$-process in AGB stars. Surprisingly, we did not detect lines from Br even though $s$-process calculations indicate that it should be produced with Kr at detectable levels.

Keywords

ISM: abundancesplanetary nebulae: generalnucleosynthesis
Type
Contributed Papers
Information
Proceedings of the International Astronomical Union , Volume 2 , Symposium S234: Planetary Nebulae in our Galaxy and Beyond , April 2006 , pp. 549 - 550
Copyright
© 2006 International Astronomical Union