The O-rich condensation sequence at low metallicity: Large Magellanic Cloud AGB and post-AGB stars

Details The O-rich condensation sequence at low metallicity: Large Magellanic Cloud AGB and post-AGB stars The O-rich condensation sequence at low metallicity: Large Magellanic Cloud AGB and post-AGB stars

Sep 2004

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2004sptz.prop.3591m&link_type=abstract

Spitzer Proposal ID #3591

Astronomy and Astrophysics

Astronomy

Scientific paper

The goal of this proposal is to study the formation and processing of dust around oxygen-rich evolved stars in the Large Magellanic Cloud (LMC). The condensation may depend heavily on the metallicity, although its effect is currently unknown. From current condensation theories it may be expected that: 1) the total condensed dust mass is lower, 2) there will be more simple oxides and less silicates, 3) the degree of crystallinity will be lower for the silicates. We propose to do IRS low resolution observations to study dust properties such as composition, grain size and shape and the dust mass distribution, to validate current condensation models. We have selected a sample of 67 oxygen-rich evolved stars in a large range of evolutionary states, ranging from red giants to planetary nebulae, in order to sample the entire dust condensation sequence. The dust in the LMC interstellar medium, as well as star forming regions in the LMC originates largely from oxygen-rich evolved stars, and therefore it is of crucial importance to know its properties. In addition, gaining an understanding of the dust condensation sequence at low metallicities will improve our understanding of dust formation in general, and will provide the ability to use grain properties and dust composition as an astronomer's tool to trace physical conditions.

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