2006/08/01 by Snežana Stanimirović, Snezana Stanimirovic
Physics and Astronomy · #Adiabatic process #Astronomy and Astrophysical Research #Astrophysics and Star Formation Studies #Focus (optics) #Luminosity #RADIUS #Shell (structure) #Stellar evolution #Stellar, planetary, and galactic studies #astro-ph
paper · pdf · doi:10.1017/s1743921307001263
in "Triggered Star Formation in a Turbulent ISM", IAU symposium 237, invited contribution
openalex publication_date 2006/08/01 · arxiv created 2006/10/12 · arxiv updated 2009/12/01 · openalex created_date 2016/06/24 · openalex updated_date 2026/08/05
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.