摘要：AbstractWe use 3D numerical simulations to study the evolution of the Hαintensity and velocity dispersion for single and multiple supernova (SN) explosions. We find that theIHα– σ diagram obtained for simulated gas flows is similar in shape to that observed in dwarf galaxies. We conclude that colliding SN shells with significant difference in age are responsible for high velocity dispersion that reaches up to ≳ 100 km s−1. Such a high velocity dispersion could be hardly obtained for a single SN remnant. Peaks of velocity dispersion in theIHα– σ diagram may correspond to several isolated or merged SN remnants with moderately different ages. Degrading the spatial resolution in the Hαintensity and velocity dispersion maps makes the simulatedIHα– σ diagrams close to those observed in dwarf galaxies not only in shape, but also quantitatively.
关键词：Keywordsgalaxies: ISMISM: bubblesISM: supernova remnantsISM: kinematics and dynamicsshock wavesmethods: numerical
