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Chemical evolution models for NGC 6822 using planetary nebulae abundances

  • Liliana Hernández-Martínez (a1) (a2), Leticia Carigi (a1), Miriam Peña (a1) and Manuel Peimbert (a1)

Abstract

We present chemical evolution models for the dwarf irregular NGC 6822, using chemical abundances of Planetary Nebulae (PNe) and HII regions and also the mass of gas (M gas ) as observational constraints. Chemical evolution models have been calculated to reproduce the abundances as derived from both, collisionally excited lines (CELs) and recombination lines (RLs). In our models, the chemical contribution of low and intermediate mass stars (LIMS) is time delayed, while for the massive stars the chemical contribution is instantaneous, as in Franco & Carigi (2008). The chemical contribution of SNIa is included in our model, thus we are also able to reproduce the observational Fe/H abundance obtained from A stars.

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Copyright

References

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Franco, I. & Carigi, L. 2008, RMAA, 44, 311.
Hernández-Martínez, L., Peña, M., Carigi, L., & García-Rojas, J., 2009, A&A, 505, 1027
Hernández-Martínez, L., Carigi, L., Peña, M., & Peimbert, M., 2011, A&A, (in press)
Talbot, R. J. Jr. & Arnett, W. D., 1971, ApJ, 170, 409.
Venn, K. A., Lennon, D. J., & Kaufer, A., 2001, ApJ, 625, 754.
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