Other
Scientific paper
Dec 1998
adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1998mcdg.proc..115b&link_type=abstract
The Magellanic Clouds and Other Dwarf Galaxies, Proceedings of the Bonn/Bochum-Graduiertenkolleg Workshop, held at the Physikzen
Other
Supergiant Shells, H Ii: Regions, Colour-Magnitude Diagrams, Star Formation, Stellar Population
Scientific paper
In this contribution I will present our project of stellar population analyses and spatial information of the Magellanic Clouds (MCs). The Large Magellanic Coud (LMC) is a suitable laboratory and testing ground for theoretical models of star formation. The distance of 50 kpc (huge compared to its depth < 300 pc) enables us to detect with today's techniques stellar light from the most massive and young stars, seen in OB associations and indirectly visible by the H II regions and H-alpha filaments, down to the low mass end of about 1/10 of a solar mass. Having a first glance at photographs of the MCs in the optical, the young population (< 25 Myr) with the associated emission nebulae (like the impressive 30 Dor region) and the large ring-like structures of about 800 pc diameters, the so called supergiant shells (SGSs), catch the eye. Despite being relatively well studied objects, these young features do not fit in a simple picture of stellar evolution history. This article comprises the poster "Stellar content of supergiant shells in the LMC" dealing with an age analysis through a CCD photometry of the inner part of SGS LMC 4 and the talk "Large-scale star formation and the bow-shock trigger scenario", which introduces a new model for the origin of the stellar structures at the LMC outskirts.
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