id	author	title	date	pages	extension	mime	words	sentences	flesch	summary	cache	txt
work_3ttdssy7lbcxldjgcindmn75na	Randall L. Cooper	Energy Crisis in the Superbubble DEM L192 (N51D)	2004	22	.pdf	application/pdf	6848	615	79	the stellar energy feedback problem because the stellar energy input can be estimated from the observed stellar content of the OB associations and the interstellar thermal and kinetic energies of superbubbles are well-defined and easy to of the hot superbubble interior and the kinetic energies of the ionized and neutral gas in the keV energy band, which includes most of the diffuse X-ray emission from DEM L 192. In our best-fit model for the diffuse X-rays from DEM L 192, the thermal component The observed flux of diffuse X-ray emission from DEM L 192 For a superbubble like DEM L 192, we expect the stellar mechanical energy injected into H I mass and the expansion velocity of the superbubble shell; the resulting kinetic energy is Fig. 2.— XMM-Newton EPIC/pn spectrum of the diffuse X-ray emission from DEM L 192. Total energy observed in the superbubble 6 ± 2	./cache/work_3ttdssy7lbcxldjgcindmn75na.pdf	./txt/work_3ttdssy7lbcxldjgcindmn75na.txt