Shells in the Magellanic System

Abstract

Abstract. The Magellanic System harbors > 800 expanding shells of neutral hydrogen, providing a unique opportunity for statistical investigations. Most of these shells are surprisingly young, 2-10 Myr old, and correlate poorly with young stellar populations. I summarize what we have learned about shell properties and particularly focus on the puzzling correlation between the shell radius and expansion velocity. In the framework of the standard, adiabatic model for shell evolution this tight correlation suggests a coherent burst of star formation across the whole Magellanic System. However, more than one mechanism for shell formation may be taking place.

ASAP – A sub-sampling approach for preserving topological structures modeled with geodesic topographic mapping

“…Similar to real dwarfs simulated irregular galaxies have a very clumpy ISM and holes due to supernovae visible in the gas density distribution [19,20]. The characterization of the distribution of supernova shells in the ISM (so-called superbubbles), and the energies of the expanding shells [21,22], can shed light on the feedback physical processes. Superbubbles are of great astronomical interest but typically measured by eye in available catalogues and automatic tools are highly desirable.…”