Astronomy and Astrophysics – Astrophysics
Scientific paper
Jan 1986
adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1986ap%26ss.118..383m&link_type=abstract
(IAU, Asian-Pacific Regional Meeting, 3rd, Kyoto, Japan, Sept. 30-Oct. 5, 1984) Astrophysics and Space Science (ISSN 0004-640X),
Astronomy and Astrophysics
Astrophysics
13
Interstellar Gas, Spiral Galaxies, Stellar Mass Ejection, Stellar Radiation, Stellar Winds, Supernova Remnants, H Ii Regions, Morphology, Stellar Evolution, Thermal Stability
Scientific paper
Stars inject energy into the interstellar medium (ISM) by radiation, stellar winds, and supernova explosions. This energy injection causes the ISM to be inhomogeneous, which in turn alters the manner in which the energy is transferred through the ISM. A significant fraction of the energy is injected by massive stars, which form H II regions in the ISM. The structure and evolution of H II regions in a cloudy medium differs significantly from that in a homogeneous one. The strong stellar winds produced by massive stars form bubbles in the ISM, and the structure of these bubbles is often dominated by the structure of the H II region in which they are embedded. Finally, when the star explodes as a supernova, the evolution and appearance of the resulting remnant is determined by the structure of the bubble and H II region formed by the star during its lifetime.
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