The Astrophysical Journal | VOL. 500

Energy Input and Mass Redistribution by Supernovae in the Interstellar Medium

Publication Date Jun 10, 1998


We present the results of numerical studies of supernova remnant evolution and its effects on galactic and globular cluster evolution. We show that parameters such as the density and the metallicity of the environment significantly influence the evolution of the remnant and thus change its effects on the global environment (e.g., globular clusters, galaxies) as a source of thermal and kinetic energy. We conducted our studies using a one-dimensional hydrodynamics code, in which we implemented a metallicity-dependent cooling function. Global time-dependent quantities such as the total kinetic and thermal energies and the radial extent are calculated for a grid of parameter sets. The quantities calculated are the total energy, the kinetic energy, the thermal energy, the radial extent, and the mass. We distinguished between the hot, rarefied bubble and the cold, dense shell, since these two phases are distinct in their roles in a gas-stellar system. We also present power-law fits to those quantities as a function of environmental parameters after the extensive cooling has ceased. The power-law fits enable simple incorporation of improved supernova energy input and matter redistribution (including the effect of the local conditions) in galactic/globular cluster models. Our results for the energetics of supernova remnants in the late stages of their expansion give total energies ranging from ≈ 9 × 1049 to ≈ 3 × 1050 ergs, with a typical case being ≈ 1050 ergs, depending on the surrounding environment. About 8.5 × 1049 ergs of this...


Kinetic Energy Thermal Energy Initial Explosion Energy Radial Extent Energy Input Thermal Energies Total Energies Globular Cluster Evolution Total Energy Input Matter Redistribution

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