It is proposed that H2O masers in star-forming regions occur early in the expansion of thin shells swept up by high-velocity winds from young massive stars. ^In W49N, confinement of the shell by a density distribution with an axial cavity can explain both the velocity field and the shape of the mass distribution. ^A modified version of the thin-shell code of Mac Low and McCray (1988), including radiation cooling, is used to model dynamically the expanding shell. ^(AIAA)
CITATION STYLE
Mac Low, M.-M., & Elitzur, M. (1993). Origin of water masers in W49N (pp. 172–175). https://doi.org/10.1007/3-540-56343-1_236
Mendeley helps you to discover research relevant for your work.