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The most oxygen-poor planetary nebula: AGB nucleosynthesis at low metallicities

Published online by Cambridge University Press:  09 March 2010

G. Stasińska ,
C. Morisset ,
G. Tovmassian ,
T. Rauch  and
T. Decressin
G. Stasińska
Affiliation:
LUTH, Observatoire de Paris, CNRS, Université Paris Diderot; Meudon, France
C. Morisset
Affiliation:
Instituto de Astronomia, Universidad Nacional Autonoma de Mexico, Mexico, Mexico
G. Tovmassian
Affiliation:
Instituto de Astronomia, Universidad Nacional Autonoma de Mexico, Mexico, Mexico
T. Rauch
Affiliation:
Institute for Astronomy and Astrophysics, Eberhard Karls University, Tuebingen, Germany
T. Decressin
Affiliation:
Argelander Institute for Astronomy (AIfA), Auf dem Hügel 71, D-53121 Bonn, Germany
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Abstract

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TS01 is an exceptional planetary nebula (PN) in the Galactic halo: it is the most oxygen-poor and has a double-degenerate core with mass close to 1.4M⊙, possibly a Supernova Ia progenitor. With data from the far UV to the IR we can pin down the abundances of half a dozen of elements. The oxygen abundance is by 1.9(±0.3) dex lower than in the Sun. Standard AGB models with appropriate mass and metallicity cannot explain the observed chemical composition. We find that additional mixing, induced by stellar rotation and/or by the presence of the close companion can explain most of the features of the abundance pattern in TS01.

Keywords

ISM: planetary nebulae: individual — ISM: abundances — Stars: AGB and post-AGB – Stars: binaries
Type
Contributed Papers
Information
Proceedings of the International Astronomical Union , Volume 5 , Symposium S265: Chemical Abundances in the Universe: Connecting First Stars to Planets , August 2009 , pp. 94 - 97
Copyright
Copyright © International Astronomical Union 2010

References

Cristallo, S., Straniero, O., Gallino, R. et al. , 2009, ApJ, 696, 797CrossRefGoogle Scholar
Decressin, T., Charbonnel, C., Siess, L. et al. , 2009, arXiv:0907.5200Google Scholar
Jacoby, G. H., Feldmeier, J. J., Claver, C. F., et al. 2002, AJ, 124, 3340Google Scholar
Karakas, A. I. & Lattanzio, J. C. 2003, PASA, 20, 393Google Scholar
Morisset, C., 2006, IAUS, 234, 467CrossRefGoogle Scholar
Péquignot, D. & Tsamis, Y. 2005, A&A, 430, 187Google Scholar
Richer, M. G., Tovmassian, G., Stasińska, G. et al. , 2002, A&A, 395, 929Google Scholar
Stasińska, G., Tovmassian, G. H., Richer, , et al. , 2005, IAUS, 228, 323Google Scholar
Stasińska, et al. 2009, A&A in pressGoogle Scholar
Tovmassian, G. H., Stasińska, G., Chavushyan, V. H., et al. , 2001, A&A, 370, 456Google Scholar
Tovmassian, G. H., Napiwotzki, R., Richer, M. G., et al. , 2004, ApJ, 616, 485CrossRefGoogle Scholar
Tovmassian, et al. 2009, ApJ submittedGoogle Scholar