Planetary Nebulae in the Magellanic Clouds: II) Abundances and element production

TL;DR

This study analyzes elemental abundances in planetary nebulae of the Magellanic Clouds to understand stellar evolution and nucleosynthesis, highlighting the effects of metallicity and challenges in initial composition estimation.

Contribution

It provides a homogeneous analysis of 183 planetary nebulae, revealing oxygen and neon production processes and their dependence on environment metallicity, with implications for stellar evolution models.

Findings

Oxygen variations due to ON cycle and production in some nebulae.

Neon production observed, linked to core or shell burning.

Sulfur and argon are reliable for initial composition estimates.

Abstract

We present the second part of an optical spectroscopic study of planetary nebulae in the LMC and SMC. The first paper, Leisy & Dennefeld (1996), discussed the CNO cycle for those objects where C abundances were available. In this paper we concentrate more on other elemental abundances (such as O, Ne, S, Ar) and their implications for the evolution of the progenitor stars. We use a much larger sample of 183 objects, of which 65 are from our own observations, where the abundances have been re-derived in a homogeneous way. For 156 of them, the quality of data is considered to be satisfactory for further analysis. We confirm the difficulty of separating Type-I and non-type-I objects in the classical He-N/O diagram, as found in Paper I, a problem reinforced by the variety of initial compositions for the progenitor stars. We observed oxygen variations, either depletion via the ON cycle in the more massive progenitor stars, or oxygen production in other objects. Neon production also appears to be present. These enrichments are best explained by fresh material from the core or from burning shells, brought to the surface by the 3rd dredge-up, as reproduced in recent models, some including overshooting. All the effects appear stronger in the SMC, suggesting a higher efficiency in a low metallicity environment. Neither oxygen nor neon can therefore be used to derive the initial composition of the progenitor star: other elements not affected by processing such as sulfur, argon or, if observed, chlorine, have to be preferred for this purpose. Some objects with very low initial abundances are detected, but on average, the spatial distribution of PNe abundances is consistent with the history of star formation (SF) as derived from field stars in both Clouds.