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| Paper: |
Quantifying Stellar Energy Feedback |
| Volume: |
331, Extra-Planar Gas |
| Page: |
297 |
| Authors: |
Chu, Y.-H. |
| Abstract: |
Massive stars inject energy into the ISM and alter the spatial distribution and physical conditions of the ISM. Two types of stellar energy need to be considered: radiation energy and mechanical energy. Stellar radiation can ionize the ISM and heat the dust. Stellar mechanical energy, i.e., fast stellar winds and supernova explosions, shock the ISM into regular shell structures as well as irregular turbulent structures. To study how stellar energy is deposited into the ISM, multi-wavelength observations are needed and Hubble, Spitzer, Chandra, XMM-Newton, and FUSE provide the necessary means for such a study. Star formation regions in the Antennae Galaxies and the Large Magellanic Cloud are used to analyze quantitatively the stellar energy feedback processes. The results illustrate that stellar energy feedback has no simple recipe and that theoretical models of super-bubble formation/evolution need to take into account micro plasma physics. |
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