Computer Science
Scientific paper
Jan 1993
adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1993egte.conf..332m&link_type=abstract
In NASA. Ames Research Center, The Evolution of Galaxies and Their Environment p 332-333 (SEE N93-26706 10-90)
Computer Science
Galactic Evolution, High Temperature Gases, Interstellar Matter, Massive Stars, Star Formation, Stellar Evolution, Stellar Mass, Stellar Winds, Supernova 1987A, Halos, Magellanic Clouds, Milky Way Galaxy, Shock Fronts, Star Clusters, Stellar Models
Scientific paper
Stars in the 9-40 solar mass range play a prominent role in the hydrodynamical and chemical evolution of galaxies. Their stellar winds and supernova explosions are believed to create the hot component of the interstellar medium (ISM). In some galactic disks, the kiloparsec sized super bubbles formed around clusters of massive stars may blow out of the disk plane and release hot, metal enriched gas into the galaxy's halo. Additionally, the expanding shock front of a super bubble in the disk may trigger additional star formation. Furthermore, similar processes probably drive the galactic winds associated with star burst nuclei that enrich the intracluster and intergalactic mediums. Nonetheless, the explosion of a blue super giant in the Large Magellanic Cloud (LMC), SN1987A, illuminated the incompleteness of our understanding of massive stars. Evolutionary models of massive stars do not synthesize the observed super giant populations in either the Milky Way or LMC. Our modeling of the formation of SN1987A's ring will improve our knowledge of both the post-main-sequence evolution of massive stars and their coupling to the ISM in galaxies.
Arnett David
Martin Crystal L.
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